Corrective Action Investigation Plan for Corrective Action Unit 168: Areas 25 and 26 Contaminated Materials and Waste Dumps, Nevada Test Site, Nevada (Rev. 0) includes Record of Technical Change No. 1 (dated 8/28/2002), Record of Technical Change No. 2 (dated 9/23/2002), and Record of Technical Change No. 3 (dated 6/2/2004)

DOE Office of Scientific and Technical Information (OSTI.GOV)

U.S. Department of Energy, National Nuclear Security Administration Nevada

This Corrective Action Investigation Plan contains the U.S. Department of Energy, National Nuclear Security Administration Nevada Operations Office's approach to collect data necessary to evaluate corrective action alternatives appropriate for the closure of Corrective Action Unit 168 under the Federal Facility Agreement and Consent Order. Corrective Action Unit 168 consists of a group of twelve relatively diverse Corrective Action Sites (CASs 25-16-01, Construction Waste Pile; 25-16-03, MX Construction Landfill; 25-19-02, Waste Disposal Site; 25-23-02, Radioactive Storage RR Cars; 25-23-18, Radioactive Material Storage; 25-34-01, NRDS Contaminated Bunker; 25-34-02, NRDS Contaminated Bunker; CAS 25-23-13, ETL - Lab Radioactive Contamination; 25-99-16, USW G3;more » 26-08-01, Waste Dump/Burn Pit; 26-17-01, Pluto Waste Holding Area; 26-19-02, Contaminated Waste Dump No.2). These CASs vary in terms of the sources and nature of potential contamination. The CASs are located and/or associated wit h the following Nevada Test Site (NTS) facilities within three areas. The first eight CASs were in operation between 1958 to 1984 in Area 25 include the Engine Maintenance, Assembly, and Disassembly Facility; the Missile Experiment Salvage Yard; the Reactor Maintenance, Assembly, and Disassembly Facility; the Radioactive Materials Storage Facility; and the Treatment Test Facility Building at Test Cell A. Secondly, the three CASs located in Area 26 include the Project Pluto testing area that operated from 1961 to 1964. Lastly, the Underground Southern Nevada Well (USW) G3 (CAS 25-99-16), a groundwater monitoring well located west of the NTS on the ridgeline of Yucca Mountain, was in operation during the 1980s. Based on site history and existing characterization data obtained to support the data quality objectives process, contaminants of potential concern (COPCs) for CAU 168 are primarily radionuclide; however, the COPCs for several CASs were not defined. To address COPC uncertainty, the analytical program for most CASs will include volatile organic compounds, semivolatile organic compounds, Resource Conservation and Recovery Act metals, total petroleum hydrocarbons, polychlorinated biphenyls, and radionuclides. Upon reviewing historical data and current site conditions, it has been determined that no further characterization is required at USW G3 (CAS 25-99-16) to select the appropriate corrective action. A cesium-137 source was encased in cement within the vadous zone during the drilling of the well (CAS 25-99-16). A corrective action of closure in place with a land-use restriction for drilling near USW G3 is appropriate. This corrective action will be documented in the Corrective Action Decision Document (CADD) for CAU 168. The results of the remaining field investigation will support a defensible evaluation of corrective action alternatives for the other CASs within CAU 168 in this CADD.« less

KSC-05pd2634

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - New Horizons leaves the Payload Hazardous Servicing Facility before dawn for its journey to the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2635

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - Technicians prepare to move New Horizons before dawn from the Payload Hazardous Servicing Facility to the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2528

NASA Image and Video Library

2005-11-29

KENNEDY SPACE CENTER, FLA. - In the Vertical Integration Facility on Launch Complex 41 at Cape Canaveral Air Force Station in Florida, workers maneuver the fifth and final solid rocket booster into place for mating to the Lockheed Martin Atlas V rocket. Two of the other four rockets are seen at left. The Atlas V is the launch vehicle for the Pluto-bound New Horizons spacecraft that will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon’s surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

KSC-05pd2312

NASA Image and Video Library

2005-10-07

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, a technician from the Applied Physics Laboratory works on the New Horizons spacecraft before installing one of the panels. A series of interconnecting panels will enclose the spacecraft beneath the antenna to maintain safe operating temperatures in space. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

KSC-05pd2311

NASA Image and Video Library

2005-10-07

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, technicians from the Applied Physics Laboratory work on a panel they are installing on the New Horizons spacecraft. A series of interconnecting panels will enclose the spacecraft beneath the antenna to maintain safe operating temperatures in space. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

KSC-05pd2314

NASA Image and Video Library

2005-10-07

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, technicians from the Applied Physics Laboratory install another panel on the New Horizons spacecraft. A series of interconnecting panels will enclose the spacecraft beneath the antenna to maintain safe operating temperatures in space. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

KSC-05pd2315

NASA Image and Video Library

2005-10-07

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, technicians from the Applied Physics Laboratory install another panel on the New Horizons spacecraft. A series of interconnecting panels will enclose the spacecraft beneath the antenna to maintain safe operating temperatures in space. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

KSC-05pd2313

NASA Image and Video Library

2005-10-07

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, technicians work on a panel they are installing on the New Horizons spacecraft. A series of interconnecting panels will enclose the spacecraft beneath the antenna to maintain safe operating temperatures in space. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

Closure of the R Reactor Disassembly Basin at the SRS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Austin, W.E.

The Facilities Disposition Division (FDD) at the Savannah River Site is engaged in planning the deactivation/closure of three of the site's five reactor disassembly basins. Activities are currently underway at R-Reactor Disassembly Basin and will continue with the P and C disassembly basins. The basins still contain the cooling and shielding water that was present when operations ceased. Low concentrations of radionuclides are present, with tritium, Cs-137, and Sr-90 being the major contributors. Although there is no evidence that any of the basins have leaked, the 50-year-old facilities will eventually contaminate the surrounding groundwaters. The FDD is pursuing a pro-activemore » solution to close the basins in-place and prevent a release to the groundwater. In-situ ion exchange is currently underway at the R-Reactor Disassembly Basin to reduce the Cs and Sr concentrations to levels that would allow release of the treated water to previously used on-site cooling ponds or to prevent ground water impact. The closure will be accomplished under CERCLA.« less

Deactivation of the P, C, and R Reactor Disassembly Basins at the SRS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Pickett, J.B.

The Facilities Disposition Division (FDD) at the Savannah River Site is engaged in planning the deactivation/closure of three of the site's five reactor disassembly basins. Activities are currently underway at 105-R Disassembly Basin and will continue with the 105-P and 105-C disassembly basins. The basins still contain the cooling and shielding water that was present when operations ceased. Low concentrations of radionuclides are present, with tritium, Cs-137, and Sr-90 being the major contributors. Although there is no evidence that any of the basins have leaked, the 50-year-old facilities will eventually contaminate the surrounding groundwaters. The FDD is pursuing a pro-activemore » solution to close the basins in-place and prevent a release to the groundwater. In-situ ion-exchange is currently underway at the R-Reactor Disassembly Basin to reduce the Cs and Sr concentrations to levels that would allow release of the treated water to previously used on-site cooling ponds. A NEPA Environmental Assessment (EA) is being prepared to propose the preferred closure alternative for each of the three basins. The EA will be the primary mechanism to inform the public and gain stakeholder and regulatory approval.« less

Deactivation of the P, C, and R Reactor Disassembly Basins at the SRS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Pickett, J.B.

The Facilities Disposition Division (FDD) at the Savannah River Site is engaged in planning the deactivation/closure of three of the site's five reactor disassembly basins. Activities are currently underway at 105-R Disassembly Basin and will continue with the 105-P and 105-C disassembly basins. The basins still contain the cooling and shielding water that was present when operations ceased. Low concentrations of radionuclides are present, with tritium, Cs-137, and Sr-90 being the major contributors. Although there is no evidence that any of the basins have leaked, the 50-year-old facilities will eventually contaminate the surrounding groundwaters. The FDD is pursuing a pro-activemore » solution to close the basins in-place and prevent a release to the groundwater. In-situ ion-exchange is currently underway at the R-Reactor Disassembly Basin to reduce the Cs and Sr concentrations to levels that would allow release of the treated water to previously used on-site cooling ponds. A NEPA Environm ental Assessment (EA) is being prepared to propose the preferred closure alternative for each of the three basins. The EA will be the primary mechanism to inform the public and gain stakeholder and regulatory approval.« less

1. GENERAL VIEW TO THE WEST OF THE EMAD FACILITY ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. GENERAL VIEW TO THE WEST OF THE E-MAD FACILITY AND THE SURROUNDING ENVIRONMENTAL AND TOPOGRAPHICAL SETTING. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

KSC-05pd2409

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, the New Horizons spacecraft is shrouded in insulating blankets that were installed to serve as a heat shield. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2407

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, a technician from the Applied Physics Laboratory adjusts part of the blanket that is being installed as a heat shield around the New Horizons spacecraft. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2632A

NASA Image and Video Library

2005-12-16

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, technicians monitor New Horizons as it is lowered onto a transporter for its move to Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2408a

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, a technician from the Applied Physics Laboratory adjusts the blanket that is being installed as a heat shield around the New Horizons spacecraft. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2407a

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, a technician from the Applied Physics Laboratory adjusts the blanket that is being installed as a heat shield around the New Horizons spacecraft. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2636

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - A Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility awaits the arrival of New Horizons at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2633

NASA Image and Video Library

2005-12-16

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, New Horizons sits atop a transporter awaiting its move to Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2625

NASA Image and Video Library

2005-12-15

KENNEDY SPACE CENTER, FLA. - The mission decal for New Horizons is laid out in strips on the floor of the Payload Hazardous Servicing Facility before installation onto the spacecraft's fairing. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2637

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - New Horizons arrives at the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station where buildup of its Lockheed Martin Atlas V launch vehicle is complete. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2639

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing lifting fixture is secured to the nose of the fairing enclosing New Horizons at the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2630

NASA Image and Video Library

2005-12-16

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, technicians prepare to lift New Horizons to a transporter for its move to Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2642

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing enclosing New Horizons arrives at the top of a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2406

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, technicians from the Applied Physics Laboratory are installing blankets that serve as heat shields around the New Horizons spacecraft. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

Highly Selective Nuclide Removal from the R-Reactor Disassembly Basin at the SRS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Pickett, J. B.; Austin, W. E.; Dukes, H. H.

This paper describes the results of a deployment of highly selective ion-exchange resin technologies for the in-situ removal of Cs-137 and Sr-90 from the Savannah River Site (SRS) R-Reactor Disassembly Basin. The deployment was supported by the DOE Office of Science and Technology's (OST, EM-50) National Engineering Technology Laboratory (NETL), as a part of an Accelerated Site Technology Deployment (ASTD) project. The Facilities Decontamination and Decommissioning (FDD) Program at the SRS conducted this deployment as a part of an overall program to deactivate three of the site's five reactor disassembly basins.

Highly Selective Nuclide Removal from the R-Reactor Disassembly Basin at SRS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Pickett, J.B.

This paper describes the results of a deployment of highly selective ion-exchange resin technologies for the in-situ removal of Cs-137 and Sr-90 from the Savannah River Site (SRS) R-Reactor Disassembly Basin. The deployment was supported by the DOE Office of Science and Technology's (OST, EM-50) National Engineering Technology Laboratory (NETL), as a part of an Accelerated Site Technology Deployment (ASTD) project. The Facilities Decontamination and Decommissioning (FDD) Program at the SRS conducted this deployment as a part of an overall program to deactivate three of the site's five reactor disassembly basins

Disney characters greet prime ASTP crewmen to Florida's Disney World

NASA Technical Reports Server (NTRS)

1975-01-01

Two Walt Disney comic cartoon characters, Donald Duck and Pluto, were on hand to greet a group of Apollo-Soyuz Test Project crewmen on their arrival at Disney World near Orlando. From left, are interpreter K. S. Samofal, interpreter Nicholas Timacheff, Cosmonaut Vladimir A. Shatalov, Astronaut Vance D. Brand, Astronaut Donald K. Slayton, Cosmonaut Aleksey A. Leonov (squeezing Pluto's nose) and Astronaut Thomas P. Stafford. The astronauts and cosmonauts were in Florida for a three-day inspection tour of the Kennedy Space Center where they looked over ASTP launch facilities and flight hardware.

KSC-05pd2412

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility is NASA’s New Horizons spacecraft that is scheduled to be launched to Pluto and its moon Charon in January 2006. Seen here is the Radio Science Experiment (REX) that will measure atmospheric composition and temperature. The spacecraft is being prepared for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2592

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, clean-suit garbed workers secure the fairing sections around the New Horizons spacecraft for encapsulation. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2641

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing lifting fixture raises the fairing enclosing New Horizons to the top of a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2646

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing enclosing New Horizons awaits further processing upon its arrival atop a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2408

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - At NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, a technician from the Applied Physics Laboratory adjusts part of the blanket that it is being installed as a heat shield around the New Horizons spacecraft. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2628

NASA Image and Video Library

2005-12-15

KENNEDY SPACE CENTER, FLA. - Technicians install strips of the New Horizons mission decal on the spacecraft fairing in the Payload Hazardous Servicing Facility. The last strip will be installed on the fairing after the spacecraft is delivered to Pad 41 on Dec. 17. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-06pd0009

NASA Image and Video Library

2006-01-11

KENNEDY SPACE CENTER, FLA. - In the Vertical Integration Facility on Launch Complex 41, Cape Canaveral Air Force Station, Hal Weaver, New Horizons project scientist with the Johns Hopkins University Applied Physics Laboratory, signs the fairing enclosing the New Horizons spacecraft. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2644

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - Technicians monitor the fairing enclosing New Horizons as it is lowered onto the top of a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2647

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing enclosing New Horizons awaits further processing upon its arrival atop a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2645

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - Technicians monitor the fairing enclosing New Horizons as it is positioned atop a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2590

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, the two fairing sections move into place around the New Horizons spacecraft for encapsulation. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2629

NASA Image and Video Library

2005-12-15

KENNEDY SPACE CENTER, FLA. - Technicians install strips of the New Horizons mission decal on the spacecraft fairing in the Payload Hazardous Servicing Facility. The last strip will be installed on the fairing after the spacecraft is delivered to Pad 41 on Dec. 17. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2591

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, the two fairing sections close in around the New Horizons spacecraft to encapsulate it. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2627

NASA Image and Video Library

2005-12-15

KENNEDY SPACE CENTER, FLA. - Technicians install strips of the New Horizons mission decal on the spacecraft fairing in the Payload Hazardous Servicing Facility. The last strip will be installed on the fairing after the spacecraft is delivered to Pad 41 on Dec. 17. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2589

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, the New Horizons spacecraft waits for encapsulation within the fairing sections waiting nearby. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2640

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing lifting fixture lifts the fairing enclosing New Horizons to the top of a Lockheed Martin Atlas V launch vehicle at the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

32. INTERIOR VIEW TO THE NORTH OF THE FIRST FLOOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

32. INTERIOR VIEW TO THE NORTH OF THE FIRST FLOOR EAST CORRIDOR AND VIEWING GALLERY TO THE DISASSEMBLY BAY. A VIEWING AND WORK STATION FOR THE EAST SIDE OF THE UPPER LEVEL OF THE DISASSEMBLY BAY IS ON THE WEST SIDE OF THE CORRIDOR. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

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NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - The fairing lifting fixture is lowered toward the nose of the fairing enclosing New Horizons upon its arrival at the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. A Lockheed Martin Atlas V launch vehicle stands ready to receive it in the background. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2588

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, the two fairing sections are ready to be moved in place around the New Horizons spacecraft (in center) for encapsulation. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2631

NASA Image and Video Library

2005-12-16

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, technicians lift New Horizons toward a transporter for its move to Complex 41 on Cape Canaveral Air Force Station. The last strip of the mission decal will be installed on the fairing after the spacecraft is delivered to the pad. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2587

NASA Image and Video Library

2005-12-13

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, clean-suit garbed workers prepare the first fairing section (in the background) that will encapsulate the New Horizons spacecraft at left for flight. The fairing protects the spacecraft during launch and flight through the atmosphere. Once out of the atmosphere, the fairing is jettisoned. The compact 1,060-pound New Horizons probe carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2632

NASA Image and Video Library

2005-12-16

KENNEDY SPACE CENTER, FLA. - In the Payload Hazardous Servicing Facility, technicians lower New Horizons onto a transporter for its move to Complex 41 on Cape Canaveral Air Force Station. The last strip of the mission decal will be installed on the fairing after the spacecraft is delivered to the pad. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2643

NASA Image and Video Library

2005-12-17

KENNEDY SPACE CENTER, FLA. - InDyne employee Mic Miracle captures on video the arrival of the fairing enclosing New Horizons at the top of a Lockheed Martin Atlas V launch vehicle in the Vertical Integration Facility at Complex 41 on Cape Canaveral Air Force Station. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

KSC-05pd2626

NASA Image and Video Library

2005-12-15

KENNEDY SPACE CENTER, FLA. - A technician installs the first strip of the New Horizons mission decal on the spacecraft fairing in the Payload Hazardous Servicing Facility. The last strip will be installed on the fairing after the spacecraft is delivered to Pad 41 on Dec. 17. New Horizons carries seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015.

Disney characters greet prime ASTP crewmen to Florida's Disney World

NASA Image and Video Library

1975-02-08

S75-24114 (8-10 Feb. 1975) --- Two Walt Disney comic cartoon characters, Donald Duck and Pluto, were on hand to greet a group of Apollo-Soyuz Test Project (ASTP) crewmen on their arrival at Disney World near Orlando. From left, are interpreter K. S. Samofal, interpreter Nicholas Timacheff, cosmonaut Vladimir A. Shatalov, astronaut Vance D. Brand, astronaut Donald K. Slayton, cosmonaut Aleksey A. Leonov (squeezing Pluto's nose) and astronaut Thomas P. Stafford. The astronauts and cosmonauts were in Florida for a three-day inspection tour of NASA's Kennedy Space Center where they looked over ASTP launch facilities and flight hardware.

KSC-05pd2648

NASA Image and Video Library

2005-12-07

KENNEDY SPACE CENTER, FLA. - A Florida quarter is prepared for installation on the New Horizons spacecraft in Kennedy Space Center's Payload Hazardous Servicing Facility. The new quarter, engraved with the "Gateway to Discovery" design, will accompany New Horizons on its 3-billion-mile journey to the planet Pluto and its moon, Charon. Although appropriate for the mission to carry the coin from the state that symbolizes space exploration, it will also serve a practical purpose: scientists are using the quarter as a spin-balance weight. New Horizons comprises seven scientific instruments that will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will launch aboard a Lockheed Martin Atlas V rocket and fly by Pluto and Charon as early as summer 2015. Photo Credit: Applied Physics Laboratory/George W. Rogers III

1. EXTERIOR VIEW TO THE NORTHEAST OF A BROCK HOUSE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. EXTERIOR VIEW TO THE NORTHEAST OF A BROCK HOUSE USED FOR THE WATER FILTERING SYSTEM. - Nevada Test Site, Pluto Facility, Water Filtering System Brock House, Area 26, Wahmonie Flats, Cane Spring Road, Mercury, Nye County, NV

4. EXTERIOR VIEW TO THE NORTH OF THE WATER TOWER ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. EXTERIOR VIEW TO THE NORTH OF THE WATER TOWER AND MISCELLANEOUS EQUIPMENT ALONG THE EAST SIDE OF THE COMPOUND. - Nevada Test Site, Pluto Facility, Area 26, Wahmonie Flats, Cane Spring Road, Mercury, Nye County, NV

2. EXTERIOR VIEW TO THE NORTH OF WATER FILTERING EQUIPMENT ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. EXTERIOR VIEW TO THE NORTH OF WATER FILTERING EQUIPMENT AND BROCK HOUSES ALONG THE EAST SIDE OF THE COMPOUND. - Nevada Test Site, Pluto Facility, Area 26, Wahmonie Flats, Cane Spring Road, Mercury, Nye County, NV

3. EXTERIOR VIEW TO THE NORTHEAST OF A RAILROAD CAR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

3. EXTERIOR VIEW TO THE NORTHEAST OF A RAILROAD CAR ON THE TRACKS AND THE PARTS OF AN ENGINE STAND. - Nevada Test Site, Pluto Facility, Area 26, Wahmonie Flats, Cane Spring Road, Mercury, Nye County, NV

27. INTERIOR VIEW TO THE WEST OF ROOM 126 AT ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

27. INTERIOR VIEW TO THE WEST OF ROOM 126 AT THE NORTH END OF THE ENTRANCE HALLWAY TO THE POST-MORTEM CELLS. IN THE CEILING IS A HATCHWAY TO THE UPPER LEVEL OF ROOM 123, THE DISASSEMBLY BAY, BY WHICH PARTS OF THE NUCLEAR REACTOR WERE PASSED FOR FURTHER DISASSEMBLY IN THE VARIOUS POST-MORTEM CELLS. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

"My naturesound" - nature observations with sound recordings

PubMed Central

Runnel, Veljo; Peterson, Marko; Zirk, Allan

2017-01-01

Abstract Background Online systems for observation reporting by citizen scientists have been operating for many years. iNaturalist (California Academy of Sciences 2016), eBird (Cornell Lab of Ornithology 2016) and Observado (Observation International 2016) are well-known international systems, Artportalen (Swedish Species Information Centre 2016) and Artsobservasjoner (Norwegian Biodiversity Information Centre 2016) are Scandinavian. In addition, databases and online solutions exist that are more directly research-oriented but still offer participation by citizen scientists, such as the PlutoF (University of Tartu Natural History Museum 2016) platform. The University of Tartu Natural History Museum maintains the PlutoF platform (Abarenkov et al. 2010) for storing and managing biodiversity data, including taxon observations. In 2014, development was started to integrate an observation app "Minu loodusheli"/"My naturesound" (University of Tartu Natural History Museum 2017b) (My naturesound, Fig. 1) within PlutoF system. In 2017, an English language version of the app (University of Tartu Natural History Museum 2017c) was launched that includes nearly all major sound-producing taxon groups in its taxonomy. The application also acts as a practical tool for collecting and publishing occurrence data for the Global Biodiversity Information Facility (Global Biodiversity Information Facility 2017) in standardized Darwin Core format together with download links to the multimedia files. Although the sound recording ability of mobile phones opens new opportunities to validate taxon occurrences, current technological solutions limit the use of recordings in biodiversity research. The "My naturesound" allows the user to record taxon occurrences and to provide audio recordings as evidence. After installing the application, the user is promted to login with PlutoF system credentials or to register with PlutoF. The application is targeted primarely to citizen scientists, but researchers themselves can also use it as a tool for easy annotation of taxon occurrences. New information The dataset consists observation data of birds, amphibians and insects by citizen scientists with on site audio recordings. The dataset gives the possibility to analyze the suitablility of mobile devices for recording animal vocalizations and their use in reporting. PMID:29104438

High Resolution HST Images of Pluto and Charon

NASA Astrophysics Data System (ADS)

1994-05-01

At the Edge of the Solar System Click here to jump to photo. The remote planet Pluto and its moon Charon orbit the Sun at a mean distance of almost 6,000 million kilometres, or nearly fourty times farther out than the Earth. During a recent investigation by an international group of astronomers [1], the best picture ever of Pluto and Charon [2] was secured with the European Space Agency's Faint Object Camera at the Hubble Space Telescope (HST). It shows the two objects as individual disks, and it is likely that further image enhancement will allow us to see surface features on Pluto. A Very Special Pair of Celestial Objects Almost all the known facts about these two bodies show that they are quite unusual: Pluto's orbit around the Sun is much more elongated and more inclined to the main plane of the Solar System than that of any other major planet; Charon's orbit around Pluto is nearly perpendicular to this plane; their mutual distance is amazingly small when compared to their size; Charon is half the size of Pluto and the ratio of their masses is much closer to unity than is the case for all other planets and their moons. Moreover, both are small and solid bodies, in contrast to the other, large and gaseous planets in the outer Solar System. We do not know why this is so. But there is another important aspect which makes Pluto and Charon even more interesting: at this very large distance from the Sun, any evolutionary changes happen very slowly. It is therefore likely that Pluto and Charon hold important clues to the conditions that prevailed in the early Solar System and thus to the origin and the evolution of the Solar System as a whole. Long and Difficult Analysis Ahead The present image shows that the overall quality of the new data obtained with the ESA Faint Object Camera on the refurbished Hubble Space Telescope is extremely good. However, such an image represents only the first step of a subsequent, detailed analysis with the ultimate goal of determining the physical properties of the two bodies, first of all their composition, surface structure and possible atmospheres. The analysis of data from a facility as complex as the Hubble Space Telescope is very demanding, and involves experts in many different fields: planetary astronomy, instrument technology, numerical image restoration, and spacecraft engineering. It is therefore not surprising that this investigation is expected to last a long time yet. However, while still in its preliminary stages, it already now appears to indicate the presence of areas of different reflectivity on the surface of Pluto. By a comparison of HST images obtained at two different wavelengths (i.e., in ultraviolet and visual light), the team members hope that it will become possible to construct rough maps of the planetary surface and perhaps also to answer the long-standing question of whether or not there is an atmosphere around Pluto. Notes: [1] This investigation is carried out at the Space Telescope European Coordinating Facility, which is located at the European Southern Observatory as part of a collaboration with the European Space Agency, and also involves other institutes in Europe and the U.S.A. The team of astronomers is headed by Rudolf Albrecht (ST-ECF), and includes Hans-Martin Adorf and Richard Hook (ST-ECF), Alessandra Gemmo and Olivier Hainaut (ESO), Cesare Barbieri and Gabriele Corrain (Osservatorio Astronomico di Padova, Italy), Chris Blades, Perry Greenfield and William Sparks (Space Telescope Science Institute, Baltimore, Maryland, U.S.A.) and David Tholen (Institute for Astronomy, University of Hawaii, U.S.A.). [2] The photo is available to the media from the ESO Information Service (address below) as ESO PR Photo 09/94-1 and from the Space Telescope Science Institute (Baltimore, USA) as STSci-PR94-17. Reproductions should be credited to NASA, ESA and ESO. Figure Caption Hubble Portrait of the "Double Planet" Pluto & Charon This is the clearest view yet of the distant planet Pluto and its moon, Charon, as revealed by the Hubble Space Telescope (HST). The image was taken by the European Space Agency's Faint Object Camera on February 21, 1994, when the planet was 4,400 million kilometres from the Earth; or nearly 30 times the separation between the Earth and the Sun. The HST corrected optics show the two objects as clearly separate and sharp disks. This now allows astronomers to measure directly (to within about 1 percent) Pluto's diameter of 2320 kilometres and Charon's diameter of 1270 kilometres. The HST observations show that Charon is bluer than Pluto. This means that the worlds have different surface composition and structure. A bright highlight on Pluto indicates that it may have a smoothly reflecting surface layer. A detailed analysis of the HST image also suggests that there is a bright area parallel to the equator of Pluto. However, subsequent observations are needed to confirm is this feature is real. Though Pluto was discovered in 1930, Charon was not detected until 1978. This is because this moon is so close to Pluto that the two world's are typically blurred together when viewed through ground-based telescopes. The new HST image was taken when Charon was near its maximum elongation from Pluto (0.9 arcseconds). The two worlds are 19,640 kilometres apart. This photo accompanies ESO PR 09/94. It is available from ESO as ESO PR Photo 09/94-1 and from the Space Telescope Science Institute (Baltimore, USA) as STSci-PR94-17. Reproductions should be credited to NASA, ESA and ESO. How to obtain ESO Press Information ESO Press Information is made available on the World-Wide Web (URL: http://www.eso.org../). ESO Press Photos may be reproduced, if credit is given to the European Southern Observatory.

The distribution of water frost on Charon

NASA Technical Reports Server (NTRS)

Buie, Marc W.; Shriver, Scott K.

1994-01-01

We present high-spatial-resolution imaging observations of the Pluto-Charon system taken with ProtoCAM on the Infrared Telescope Facility (IRTF). Our dataset consists of measurements from eight nights at widely separated rotational longitudes and covering five wavelengths -- standard J, H, and K, plus two special narrow band filters at 1.5 and 1.75 microns. The relative flux contributions of Pluto and Charon were extracted, when possible, by fitting a two-source Gaussian image model to the observed images. At K, we find the Charon-Pluto magnitude difference to be on average 1.8 mag, somewhat less than the value of 2.2 mag found by Bosh et al. (1992). The average differential magnitude at 1.5 and 1.75 microns is 2.0 and 1.6, respectively. The larger magnitude difference at 1.5 microns is due to a water-frost absorption band on the surface of Charon. Our observations are consistent with a surface of Charon dominated by water frost at all longitudes.

KSC-05pd2410

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, the New Horizons spacecraft is prepared for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Seen behind the spacecraft is one half of the fairing that will enclose it for launch, scheduled for January 2006. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2415

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, technicians prepare the New Horizons spacecraft for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Seen behind the spacecraft is one half of the fairing that will enclose it for launch, scheduled for January 2006. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2414

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, the New Horizons spacecraft is ready for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Seen behind the spacecraft is one half of the fairing that will enclose it for launch, scheduled for January 2006. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2411

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, technicians prepare the New Horizons spacecraft for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Seen behind the spacecraft is one half of the fairing that will enclose it for launch, scheduled for January 2006. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

KSC-05pd2413

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, the New Horizons spacecraft is being prepared for a media event. Photographers and reporters will be able to photograph the New Horizons spacecraft and talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Seen behind the spacecraft is one half of the fairing that will enclose it for launch, scheduled for January 2006. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

Characterization of nitrogen ice on Pluto's surface from 1-4 micron spectroscopy

NASA Astrophysics Data System (ADS)

Young, E.; Olkin, C.; Grundy, W.; Young, L.; Schmitt, B.; Tokunaga, A.; Owen, T.; Roush, T.; Terada, H.

Nitrogen ice is the predominant ice on Pluto's surface. Methane and CO have also been identified (e.g., Grundy & Buie 2001), but they are thought to be trace consituents relative to N2 , mainly because of the strength of nitrogen's 2.147 µm feature. It is assumed that the temperature of the surface N2 frost controls the column abundance of Pluto's atmosphere through vapor pressure equilibrium. The vapor pressures of CO and CH4 are about 5 and 10,000 times less than that of N2 at a typical temperature for Pluto's surface. There is spectroscopic evidence that CH4 ice exists as a dissolved constituent in a predominantly nitrogen ice matrix as well as separate, pure CH4 ice. It would be interesting to know what fraction of N2 ice is pure for purposes of modeling the surface/atmosphere interactions on Pluto. We present spectroscopic modeling to show that the fraction of pure N2 ice on Pluto is very small indeed - conservatively less than 6% by area. We will present spectral observations and modeling results from the IRTF1 , W.M. Keck2 and Subaru3 Observatories spanning 1.0 to 4.0 µm. We have implemented a Hapke model (Hapke 1993) to constrain the abundance and states of N2 ice and CH4 ice. The depth of the Pluto spectrum at 3.3 µm effectively limits the amount of pure N2 ice that can be present on Pluto. Grundy, W. M. & Buie, M. W. 2001, Icarus, 153, 248. Hapke, B. 1993, Theory of Reflectance and Emittance Spectroscopy, Cambridge Univ. Press, New York. 1 Based in part on data obtained at the Infrared Telescope Facility, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the National Aeronautics and Space Administration, Science Mission Directorate, Planetary Astronomy Program. 2 The data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The 1 Observatory was made possible by the generous financial support of the W.M. Keck Foundation. 3 Based in part on data collected at Subaru Telescope, which is operated by the National Astronomical Observatory of Japan. 2

KSC-05pd2273

NASA Image and Video Library

2005-09-29

KENNEDY SPACE CENTER, FLA. - On the Shuttle Landing Facility at NASA Kennedy Space Center, the Atlas V fairing halves for the New Horizons spacecraft have been offloaded from the Russian cargo plane (background). The fairing halves will be transported to Astrotech Space Operations in Titusville. The fairing later will be placed around the New Horizons spacecraft in the Payload Hazardous Service Facility. A fairing protects a spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. The Lockheed Martin Atlas V is the launch vehicle for the New Horizons spacecraft, which is designed to make the first reconnaissance of Pluto and Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and its moon, Charon, in July 2015.

KSC-05pd2274

NASA Image and Video Library

2005-09-29

KENNEDY SPACE CENTER, FLA. - On the Shuttle Landing Facility at NASA Kennedy Space Center, one of the Atlas V fairing halves for the New Horizons spacecraft is offloaded from the Russian cargo plane. The fairing halves will be transported to Astrotech Space Operations in Titusville. The fairing later will be placed around the New Horizons spacecraft in the Payload Hazardous Service Facility. A fairing protects a spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. The Lockheed Martin Atlas V is the launch vehicle for the New Horizons spacecraft, which is designed to make the first reconnaissance of Pluto and Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and its moon, Charon, in July 2015.

KSC-05pd2271

NASA Image and Video Library

2005-09-29

KENNEDY SPACE CENTER, FLA. - A Russian cargo plane sits on the Shuttle Landing Facility at NASA Kennedy Space Center with the Atlas V fairing for the New Horizons spacecraft inside. The two fairing halves will be removed, loaded onto trucks and transported to Astrotech Space Operations in Titusville. The fairing later will be placed around the New Horizons spacecraft in the Payload Hazardous Service Facility. A fairing protects a spacecraft during launch and flight through the atmosphere. Once in space, it is jettisoned. The Lockheed Martin Atlas V is the launch vehicle for the New Horizons spacecraft, which is designed to make the first reconnaissance of Pluto and Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and its moon, Charon, in July 2015.

ICE MINERALOGY ACROSS AND INTO THE SURFACES OF PLUTO, TRITON, AND ERIS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Tegler, S. C.; Grundy, W. M.; Olkin, C. B.

We present three near-infrared spectra of Pluto taken with the Infrared Telescope Facility and SpeX, an optical spectrum of Triton taken with the MMT and the Red Channel Spectrograph, and previously published spectra of Pluto, Triton, and Eris. We combine these observations with a two-phase Hapke model and gain insight into the ice mineralogy on Pluto, Triton, and Eris. Specifically, we measure the methane-nitrogen mixing ratio across and into the surfaces of these icy dwarf planets. In addition, we present a laboratory experiment that demonstrates it is essential to model methane bands in spectra of icy dwarf planets with twomore » methane phases-one highly diluted by nitrogen and the other rich in methane. For Pluto, we find bulk, hemisphere-averaged, methane abundances of 9.1% {+-} 0.5%, 7.1% {+-} 0.4%, and 8.2% {+-} 0.3% for sub-Earth longitudes of 10 Degree-Sign , 125 Degree-Sign , and 257 Degree-Sign . Application of the Wilcoxon rank sum test to our measurements finds these small differences are statistically significant. For Triton, we find bulk, hemisphere-averaged, methane abundances of 5.0% {+-} 0.1% and 5.3% {+-} 0.4% for sub-Earth longitudes of 138 Degree-Sign and 314 Degree-Sign . Application of the Wilcoxon rank sum test to our measurements finds the differences are not statistically significant. For Eris, we find a bulk, hemisphere-averaged, methane abundance of 10% {+-} 2%. Pluto, Triton, and Eris do not exhibit a trend in methane-nitrogen mixing ratio with depth into their surfaces over the few centimeter range probed by these observations. This result is contrary to the expectation that since visible light penetrates deeper into a nitrogen-rich surface than the depths from which thermal emission emerges, net radiative heating at depth would drive preferential sublimation of nitrogen leading to an increase in the methane abundance with depth.« less

Cape Canaveral Air Force Station, Launch Complex 39, Solid Rocket ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

Cape Canaveral Air Force Station, Launch Complex 39, Solid Rocket Booster Disassembly & Refurbishment Complex, Thrust Vector Control Deservicing Facility, Hangar Road, Cape Canaveral, Brevard County, FL

1. EXTERIOR VIEW TO THE NORTH OF THE SOUTH ELEVATIONS ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

1. EXTERIOR VIEW TO THE NORTH OF THE SOUTH ELEVATIONS OF THE R-MAD FACILITY WITH THE COLD ASSEMBLY AREA ON THE LEFT AND THE HOT DISASSEMBLY AREA TO THE RIGHT. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Projected Costs of U.S. Nuclear Forces, 2014 to 2023

DTIC Science & Technology

2013-12-01

uranium and pluto- nium, and also includes several large construction projects for new facilities to support that mission); $12 billion is for...contributed to the analysis with guidance from Sarah Jennings. Justin Falk of CBO provided helpful comments on the report, as did Russell Rumbaugh

KSC-06pd0066

NASA Image and Video Library

2006-01-16

KENNEDY SPACE CENTER, FLA. - On Complex 41 at Cape Canaveral Air Force Station, the Atlas V expendable launch vehicle with the New Horizons spacecraft rolls out of the Vertical Integration Facility on its way to the launch pad. The liftoff is scheduled for 1:24 p.m. EST Jan. 17. After its launch aboard the Atlas V, the compact, 1,050-pound piano-sized probe will get a boost from a kick-stage solid propellant motor for its journey to Pluto. New Horizons will be the fastest spacecraft ever launched, reaching lunar orbit distance in just nine hours and passing Jupiter 13 months later. The New Horizons science payload, developed under direction of Southwest Research Institute, includes imaging infrared and ultraviolet spectrometers, a multi-color camera, a long-range telescopic camera, two particle spectrometers, a space-dust detector and a radio science experiment. The dust counter was designed and built by students at the University of Colorado, Boulder. A launch before Feb. 3 allows New Horizons to fly past Jupiter in early 2007 and use the planet’s gravity as a slingshot toward Pluto. The Jupiter flyby trims the trip to Pluto by as many as five years and provides opportunities to test the spacecraft’s instruments and flyby capabilities on the Jupiter system. New Horizons could reach the Pluto system as early as mid-2015, conducting a five-month-long study possible only from the close-up vantage of a spacecraft.

KSC-06pd0072

NASA Image and Video Library

2006-01-16

KENNEDY SPACE CENTER, FLA. - On Complex 41 at Cape Canaveral Air Force Station, the Atlas V expendable launch vehicle with the New Horizons spacecraft rolls out of the Vertical Integration Facility (left) on its way to the launch pad. Liftoff is scheduled for 1:24 p.m. EST Jan. 17. After its launch aboard the Atlas V, the compact, 1,050-pound piano-sized probe will get a boost from a kick-stage solid propellant motor for its journey to Pluto. New Horizons will be the fastest spacecraft ever launched, reaching lunar orbit distance in just nine hours and passing Jupiter 13 months later. The New Horizons science payload, developed under direction of Southwest Research Institute, includes imaging infrared and ultraviolet spectrometers, a multi-color camera, a long-range telescopic camera, two particle spectrometers, a space-dust detector and a radio science experiment. The dust counter was designed and built by students at the University of Colorado, Boulder. A launch before Feb. 3 allows New Horizons to fly past Jupiter in early 2007 and use the planet’s gravity as a slingshot toward Pluto. The Jupiter flyby trims the trip to Pluto by as many as five years and provides opportunities to test the spacecraft’s instruments and flyby capabilities on the Jupiter system. New Horizons could reach the Pluto system as early as mid-2015, conducting a five-month-long study possible only from the close-up vantage of a spacecraft.

KSC-06pd0068

NASA Image and Video Library

2006-01-16

KENNEDY SPACE CENTER, FLA. - On Complex 41 at Cape Canaveral Air Force Station, the Atlas V expendable launch vehicle with the New Horizons spacecraft is being moved from the Vertical Integration Facility to the pad. The liftoff is scheduled for 1:24 p.m. EST Jan. 17. After its launch aboard the Atlas V, the compact, 1,050-pound piano-sized probe will get a boost from a kick-stage solid propellant motor for its journey to Pluto. New Horizons will be the fastest spacecraft ever launched, reaching lunar orbit distance in just nine hours and passing Jupiter 13 months later. The New Horizons science payload, developed under direction of Southwest Research Institute, includes imaging infrared and ultraviolet spectrometers, a multi-color camera, a long-range telescopic camera, two particle spectrometers, a space-dust detector and a radio science experiment. The dust counter was designed and built by students at the University of Colorado, Boulder. A launch before Feb. 3 allows New Horizons to fly past Jupiter in early 2007 and use the planet’s gravity as a slingshot toward Pluto. The Jupiter flyby trims the trip to Pluto by as many as five years and provides opportunities to test the spacecraft’s instruments and flyby capabilities on the Jupiter system. New Horizons could reach the Pluto system as early as mid-2015, conducting a five-month-long study possible only from the close-up vantage of a spacecraft.

KSC-06pd0067

NASA Image and Video Library

2006-01-16

KENNEDY SPACE CENTER, FLA. - On Complex 41 at Cape Canaveral Air Force Station, the Atlas V expendable launch vehicle with the New Horizons spacecraft rolls out of the Vertical Integration Facility on its way to the pad. The liftoff is scheduled for 1:24 p.m. EST Jan. 17. After its launch aboard the Atlas V, the compact, 1,050-pound piano-sized probe will get a boost from a kick-stage solid propellant motor for its journey to Pluto. New Horizons will be the fastest spacecraft ever launched, reaching lunar orbit distance in just nine hours and passing Jupiter 13 months later. The New Horizons science payload, developed under direction of Southwest Research Institute, includes imaging infrared and ultraviolet spectrometers, a multi-color camera, a long-range telescopic camera, two particle spectrometers, a space-dust detector and a radio science experiment. The dust counter was designed and built by students at the University of Colorado, Boulder. A launch before Feb. 3 allows New Horizons to fly past Jupiter in early 2007 and use the planet’s gravity as a slingshot toward Pluto. The Jupiter flyby trims the trip to Pluto by as many as five years and provides opportunities to test the spacecraft’s instruments and flyby capabilities on the Jupiter system. New Horizons could reach the Pluto system as early as mid-2015, conducting a five-month-long study possible only from the close-up vantage of a spacecraft.

KSC-05pd2416

NASA Image and Video Library

2005-11-04

KENNEDY SPACE CENTER, FLA. - In the clean room at KSC’s Payload Hazardous Servicing Facility, the media (also dressed in clean room suits) learn about NASA’s New Horizons spacecraft (at left) from New Horizons Mission Systems Engineer David Kusnierkiewicz, in the center. Behind Kusnierkiewicz is one half of the fairing that will enclose the spacecraft for launch, scheduled for January 2006. The media event brought photographers and reporters to the site to talk with project management and test team members from NASA and the Johns Hopkins University Applied Physics Laboratory. Carrying seven scientific instruments, the compact 1,060-pound New Horizons probe will characterize the global geology and geomorphology of Pluto and its moon Charon, map their surface compositions and temperatures, and examine Pluto's complex atmosphere. After that, flybys of Kuiper Belt objects from even farther in the solar system may be undertaken in an extended mission. New Horizons is the first mission in NASA's New Frontiers program of medium-class planetary missions. The spacecraft, designed for NASA by the Johns Hopkins University Applied Physics Laboratory in Laurel, Md., will fly by Pluto and Charon as early as summer 2015.

10. VIEW WITHIN THE EAST OPERATING GALLERY OF WORK STATION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

10. VIEW WITHIN THE EAST OPERATING GALLERY OF WORK STATION WITH MANIPULATOR ARMS. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

14. VIEW IN THE WEST OPERATING GALLERY OF POSTMORTEM CELL ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

14. VIEW IN THE WEST OPERATING GALLERY OF POST-MORTEM CELL WORK STATION AND MANIPULATOR ARMS. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

16. VIEW OF FIRST FLOOR EAST OPERATING GALLERY. NOTE THE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

16. VIEW OF FIRST FLOOR EAST OPERATING GALLERY. NOTE THE SERIES OF MANIPULATOR ARMS ALONG THE LEFT WALL. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

7. VIEW OF E5 WORK STATION AND MANIPULATOR ARMS WITHIN ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

7. VIEW OF E-5 WORK STATION AND MANIPULATOR ARMS WITHIN THE SOUTHEAST CORNER OF THE HOT BAY. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

8. EXTERIOR VIEW TO THE WEST OF THE EAST ELEVATION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. EXTERIOR VIEW TO THE WEST OF THE EAST ELEVATION OF THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

2. EXTERIOR VIEW TO THE NORTH OF THE SOUTH ELEVATION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. EXTERIOR VIEW TO THE NORTH OF THE SOUTH ELEVATION OF THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

8. VIEW OF E3 WORK STATION WITH MANIPULATOR ARMS IN ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

8. VIEW OF E-3 WORK STATION WITH MANIPULATOR ARMS IN EAST OPERATING GALLERY LOOKING INTO THE HOT BAY. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

22. INTERIOR VIEW TO THE SOUTHWEST OF THE LOWER LEVEL ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

22. INTERIOR VIEW TO THE SOUTHWEST OF THE LOWER LEVEL OF ROOM 123, THE DISASSEMBLY BAY. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

21. INTERIOR VIEW TO THE SOUTHEAST OF THE LOWER LEVEL ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

21. INTERIOR VIEW TO THE SOUTHEAST OF THE LOWER LEVEL OF ROOM 123, THE DISASSEMBLY BAY. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

6. EXTERIOR VIEW TO THE SOUTH OF THE NORTH ELEVATION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. EXTERIOR VIEW TO THE SOUTH OF THE NORTH ELEVATION OF THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

5. VIEW TO THE SOUTHEAST OF THE HOT BAY AND ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. VIEW TO THE SOUTHEAST OF THE HOT BAY AND ATTACHED OPERATING GALLERIES ALONG THE WEST SIDE OF THE BAY. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

23. INTERIOR VIEW TO THE SOUTHEAST OF THE UPPER SECTION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

23. INTERIOR VIEW TO THE SOUTHEAST OF THE UPPER SECTION OF ROOM 123, THE DISASSEMBLY BAY. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

24. INTERIOR VIEW TO THE SOUTHWEST OF THE UPPER SECTION ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

24. INTERIOR VIEW TO THE SOUTHWEST OF THE UPPER SECTION OF ROOM 123, THE DISASSEMBLY BAY. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

37. INTERIOR VIEW TO THE WEST OF ROOM 203, THE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

37. INTERIOR VIEW TO THE WEST OF ROOM 203, THE CONTROL ROOM FOR THE DISASSEMBLY BAY. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Dynamical and observational constraints on satellites in the inner Pluto-Charon system

NASA Technical Reports Server (NTRS)

Stern, S. Alan; Parker, Joel William; Duncan, Martin J.; Snowdall, J. Clark, Jr.; Levison, Harold F.

1994-01-01

It is not known if Pluto has other satellites besides its massive partner Charon. In the past, searches for additional satellites in the Pluto-Charon system have extended from the solar-tidal stability boundary (approximately 90 arcsec from Pluto) inward to about 1 arcsec from Pluto. Here we further explore the inner (i.e., less than 10 arcsec) region of the Pluto-Charon system to determine where additional satellites might lie. In particular, we report on (1) dynamical simulations to delineate the region where unstable orbits lie around Charon, (2) dynamical simulations which use the low orbital eccentricity of Charon to constrain the mass of any third body near Pluto, and (3) analysis of Hubble Space Telescope (HST) archival images to search for satellites in the inner Pluto-Charon system. Although no objects were found, significant new constraints on bodies orbiting in the inner Pluto-Charon system were obtained.

A Full View of Pluto Stunning Crescent

NASA Image and Video Library

2015-10-29

In September, NASA's New Horizons team released a stunning but incomplete image of Pluto's crescent. Thanks to new processing work by the science team, New Horizons is releasing the entire, breathtaking image of Pluto. This image was made just 15 minutes after New Horizons' closest approach to Pluto on July 14, 2015, as the spacecraft looked back at Pluto toward the sun. The wide-angle perspective of this view shows the deep haze layers of Pluto's atmosphere extending all the way around Pluto, revealing the silhouetted profiles of rugged plateaus on the night (left) side. The shadow of Pluto cast on its atmospheric hazes can also be seen at the uppermost part of the disk. On the sunlit side of Pluto (right), the smooth expanse of the informally named icy plain Sputnik Planum is flanked to the west (above, in this orientation) by rugged mountains up to 11,000 feet (3,500 meters) high, including the informally named Norgay Montes in the foreground and Hillary Montes on the skyline. Below (east) of Sputnik, rougher terrain is cut by apparent glaciers. The backlighting highlights more than a dozen high-altitude layers of haze in Pluto's tenuous atmosphere. The horizontal streaks in the sky beyond Pluto are stars, smeared out by the motion of the camera as it tracked Pluto. The image was taken with New Horizons' Multi-spectral Visible Imaging Camera (MVIC) from a distance of 11,000 miles (18,000 kilometers) to Pluto. The resolution is 700 meters (0.4 miles).

26. INTERIOR VIEW TO THE SOUTH OF ROOM 148, A ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

26. INTERIOR VIEW TO THE SOUTH OF ROOM 148, A POST-MORTEM CELL IN THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

29. INTERIOR VIEW TO THE EAST OF ROOM 144, A ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

29. INTERIOR VIEW TO THE EAST OF ROOM 144, A POST-MORTEM CELL IN THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Imagine a Landing on Pluto

NASA Image and Video Library

2016-07-14

Imagine a future spacecraft following New Horizons' trailblazing path to Pluto, but instead of flying past its target -- as New Horizons needed to do to explore Pluto and the Kuiper Belt beyond -- the next visitor touches down near the tall mountains on the frozen icy, plains of Pluto's heart. A video produced by New Horizons scientists that offers that very perspective. Made from more than 100 New Horizons images taken over six weeks of approach and close flyby, the video offers a trip in to Pluto -- starting with a distant spacecraft's-eye view of Pluto and its largest moon, Charon, to an eventual ride in for a "landing" on the shoreline of Pluto's informally named Sputnik Planum. The video shows what it would be like to ride aboard an approaching spacecraft and see Pluto grow from a "dot" to become a world, and then to swoop down over Pluto's spectacular terrains. New Horizons scientists had to interpolate some of the frames in the movie based on what they know Pluto looks like to make it as smooth and seamless as possible. After a 9.5-year voyage covering more than three billion miles, New Horizons flew through the Pluto system on July 14, 2015, coming within 7,800 miles (12,500 kilometers) of Pluto itself. Carrying powerful telescopic cameras that could spot features smaller than a football field, New Horizons has sent back hundreds of images of Pluto and its moons that show how dynamic and fascinating their surfaces are - and what great targets they'd make for follow-up mission one day. http://photojournal.jpl.nasa.gov/catalog/PIA20742

Pushing back the frontier - A mission to the Pluto-Charon system

NASA Technical Reports Server (NTRS)

Farquhar, Robert; Stern, S. Alan

1990-01-01

A flyby mission to Pluto is proposed. The size, orbit, atmosphere, and surface of Pluto, and the Pluto-Charon system are described. The benefits of a planetary flyby compared to ground observations are discussed in terms of imaging capabilities. Planned payloads include a plasma science package, a UV spectrometer, and a thermal mapper. The advantages of a dual launch to Mars and the need for a Jupiter-Pluto transfer are considered. A diagram of a spacecraft for a flyby study of Pluto is provided.

X-Rays from Pluto

NASA Image and Video Library

2016-09-14

The first detection of Pluto in X-rays has been made using NASA's Chandra X-ray Observatory in conjunction with observations from NASA's New Horizons spacecraft. As New Horizons approached Pluto in late 2014 and then flew by the planet during the summer of 2015, Chandra obtained data during four separate observations. During each observation, Chandra detected low-energy X-rays from the small planet. The main panel in this graphic is an optical image taken from New Horizons on its approach to Pluto, while the inset shows an image of Pluto in X-rays from Chandra. There is a significant difference in scale between the optical and X-ray images. New Horizons made a close flyby of Pluto but Chandra is located near the Earth, so the level of detail visible in the two images is very different. The Chandra image is 180,000 miles across at the distance of Pluto, but the planet is only 1,500 miles across. Pluto is detected in the X-ray image as a point source, showing the sharpest level of detail available for Chandra or any other X-ray observatory. This means that details over scales that are smaller than the X-ray source cannot be seen here. Detecting X-rays from Pluto is a somewhat surprising result given that Pluto - a cold, rocky world without a magnetic field - has no natural mechanism for emitting X-rays. However, scientists knew from previous observations of comets that the interaction between the gases surrounding such planetary bodies and the solar wind - the constant streams of charged particles from the sun that speed throughout the solar system -- can create X-rays. The researchers were particularly interested in learning more about the interaction between the gases in Pluto's atmosphere and the solar wind. The New Horizon spacecraft carries an instrument designed to measure that activity up-close -- Solar Wind Around Pluto (SWAP) -- and scientists examined that data and proposed that Pluto contains a very mild, close-in bowshock, where the solar wind first "meets" Pluto (similar to a shock wave that forms ahead of a supersonic aircraft) and a small wake or tail behind the planet. The immediate mystery is that Chandra's readings on the brightness of the X-rays are much higher than expected from the solar wind interacting with Pluto's atmosphere. The Chandra detection is also surprising since New Horizons discovered Pluto's atmosphere was much more stable than the rapidly escaping, "comet-like" atmosphere that many scientists expected before the spacecraft flew past in July 2015. In fact, New Horizons found that Pluto's interaction with the solar wind is much more like the interaction of the solar wind with Mars, than with a comet. While Pluto is releasing enough gas from its atmosphere to make the observed X-rays, there isn't enough solar wind flowing directly at Pluto at its great distance from the Sun to make them according to certain theoretical models. There are several suggested possibilities for the enhanced X-ray emission from Pluto. These include a much wider and longer tail of gases trailing Pluto than New Horizons detected using its SWAP instrument. Because Pluto is so small compared to the size of a Chandra point source, scientists may be unable to detect such a tail in X-rays. Other possibilities are that interplanetary magnetic fields are focusing more particles than expected from the solar wind into the region around Pluto, or the low density of the solar wind in the outer solar system at the distance of Pluto could allow for the formation of a doughnut, or torus, of neutral gas centered around Pluto's orbit. It will take deeper and higher resolution images of X-rays from Pluto's environment than we currently have from Chandra to distinguish between these possibilities. http://photojournal.jpl.nasa.gov/catalog/PIA21061

Pluto's atmosphere in 2015 from high-resolution spectroscopy

NASA Astrophysics Data System (ADS)

Roe, Henry G.; Cook, Jason C.; Mace, Gregory N.; Holler, Bryan J.; Young, Leslie A.; McLane, Jacob N.; Jaffe, Daniel T.

2015-11-01

Pluto's thin N2/CH4 atmosphere is in vapor-pressure equilibrium with ices on its surface. The atmosphere evolves seasonally with the varying insolation pattern on Pluto's heterogenous surface, perhaps even largely freezing out to the surface during the coldest portion of Pluto's year. We use high-resolution (R≈25,000-50,000) near-infrared spectroscopy to resolve atmospheric methane absorption lines from Pluto's continuum spectra, as well as separate Pluto's atmospheric lines from the telluric spectrum. In addition to measuring the abundance and temperature of Pluto's atmospheric CH4, with broad wavelength coverage we are able to search for the inevitable products of N2/CH4 photochemistry. In 2015 we are undertaking an intensive campaign using NIRSPEC at Keck Observatory and IGRINS (Immersion Grating INfrared Spectrometer) at McDonald Observatory to coincide with the New Horizons Pluto encounter. We will report initial results from this 2015 campaign and compare the state of Pluto's atmosphere at the time of the New Horizons encounter with earlier years.

Understanding facilities design parameters for a remanufacturing system

NASA Astrophysics Data System (ADS)

Topcu, Aysegul; Cullinane, Thomas

2005-11-01

Remanufacturing is rapidly becoming a very important element in the economies of the world. Products such as washing machines, clothes driers, automobile parts, cell phones and a wide range of consumer durable goods are being reclaimed and sent through processes that restore these products to levels of operating performance that are as good or better than their new product performance. The operations involved in the remanufacturing process add several new dimensions to the work that must be performed. Disassembly is an operation that rarely appears on the operations chart of a typical production facility. The inspection and test functions in remanufacturing most often involve several more tasks than those involved in the first time manufacturing cycle. A close evaluation of most any remanufacturing operation reveals several points in the process in which parts must be cleaned, tested and stored. Although several researchers have focused their work on optimizing the disassembly function and the inspection, test and store functions, very little research has been devoted to studying the impact of the facilities design on the effectiveness of the remanufacturing process. The purpose of this paper will be to delineate the differences between first time manufacturing operations and remanufacturing operations for durable goods and to identify the features of the facilities design that must be considered if the remanufacturing operations are to be effective.

13. VIEW OF EAST OPERATING GALLERY ALONG THE POSTMORTEM CELLS. ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

13. VIEW OF EAST OPERATING GALLERY ALONG THE POST-MORTEM CELLS. A NUMBER OF MANIPULATOR ARMS COVERED WITH PLASTIC ARE ON THE LEFT WALL. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

28. INTERIOR VIEW TO THE SOUTHEAST OF ROOMS 133 AND ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

28. INTERIOR VIEW TO THE SOUTHEAST OF ROOMS 133 AND 134, POST-MORTEM CELLS IN THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

20. INTERIOR VIEW TO THE EAST OF THE ACCESS RAMP ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

20. INTERIOR VIEW TO THE EAST OF THE ACCESS RAMP TO THE HOT DISASSEMBLY AREA FROM THE COLD ASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Mass-radius relationships and constraints on the composition of Pluto

NASA Technical Reports Server (NTRS)

Lupo, M. J.; Lewis, J. S.

1980-01-01

With the new upper limit of Pluto's mass, an upper limit for Pluto's density of 1.74 g/cu cm has been found. Assuming Pluto to be 100% methane, available methane density data can be used to set a lower limit of 0.53 g/cu cm on Pluto's density, thus placing an absolute upper limit of 1909 km on the radius and a lower limit of 0.32 on the albedo. The results of 280 computer models covering a wide range of composition ratios of rock, water ice, and methane ice are reported. Limits are placed on Pluto's silicate content, and a simple spacecraft method for determining Pluto's water content from its density and moment of inertia is given. The low thermal conductivity and strength of solid methane suggest rapid solid-state convection in Pluto's methane layer.

Pluto Color Map

NASA Image and Video Library

2017-01-20

This new, detailed global mosaic color map of Pluto is based on a series of three color filter images obtained by the Ralph/Multispectral Visual Imaging Camera aboard New Horizons during the NASA spacecraft's close flyby of Pluto in July 2015. The mosaic shows how Pluto's large-scale color patterns extend beyond the hemisphere facing New Horizons at closest approach- which were imaged at the highest resolution. North is up; Pluto's equator roughly bisects the band of dark red terrains running across the lower third of the map. Pluto's giant, informally named Sputnik Planitia glacier - the left half of Pluto's signature "heart" feature -- is at the center of this map. http://photojournal.jpl.nasa.gov/catalog/PIA11707

Pluto in Hi-Def Note: There is debate within the science community as to whether Pluto should be

NASA Technical Reports Server (NTRS)

2008-01-01

This image demonstrates the first detection of Pluto using the high-resolution mode on the New Horizons Long-Range Reconnaissance Imager (LORRI). The mode provides a clear separation between Pluto and numerous nearby background stars. When the image was taken on October 6, 2007, Pluto was located in the constellation Serpens, in a region of the sky dense with background stars.

Typically, LORRI's exposure time in hi-res mode is limited to approximately 0.1 seconds, but by using a special pointing mode that allowed an increase in the exposure time to 0.967 seconds, scientists were able to spot Pluto, which is approximately 15,000 times fainter than human eyes can detect.

New Horizons was still too far from Pluto (3.6 billion kilometers, or 2.2 billion miles) for LORRI to resolve any details on Pluto's surface that won't happen until summer 2014, approximately one year before closest approach. For now the entire Pluto system remains a bright dot to the spacecraft's telescopic camera, though LORRI is expected to start resolving Charon from Pluto seeing them as separate objects in summer 2010.

Energetic Particles in the far and near Environment of Pluto

NASA Astrophysics Data System (ADS)

Kollmann, P.; Hill, M. E.; McNutt, R. L., Jr.; Brown, L. E.; Kusterer, M. B.; Vandegriff, J. D.; Smith, H. T.; Mitchell, D. G.; Haggerty, D. K.; Bagenal, F.; Krimigis, S. M.; Lisse, C. M.; Delamere, P. A.; Elliott, H. A.; Horanyi, M.; McComas, D. J.; Piquette, M. R.; Poppe, A. R.; Sidrow, E. J.; Strobel, D. F.; Szalay, J.; Valek, P. W.; Weidner, S.; Zirnstein, E.; Ennico Smith, K.; Olkin, C.; Weaver, H. A., Jr.; Young, L. A.; Stern, A.

2015-12-01

The New Horizons spacecraft was launched in 2006, passed Jupiter and its magnetotail, took continuous measurements in the solar wind throughout the recent years, and flew by Pluto in July 2015. The onboard PEPSSI instrument measures ion and electron intensities, masses, and energies in the keV to MeV range. The closest approach distance to Pluto was 11 Pluto radii, inside the orbit of Charon. Data taken near Pluto is downlinked throughout August. We will present analysis of this data and set it into context with previous measurements. We expect a number of interesting particle structures around Pluto. Parts of Pluto's molecular nitrogen atmosphere is escaping and will co-orbit with Pluto, potentially forming a partial gas torus. This torus can be additionally sourced by other Kuiper belt objects. The neutrals are eventually ionized and pick-up by the solar wind brings them into the PEPSSI energy range. The measured ion densities can be used to constrain the Pluto torus. Pluto is not expected to have an intrinsic magnetic field, but the energetic particle data can be used to infer its properties, if any. Pluto interacts instead with the solar wind via the pick-up of its ions and the magnetic fields created by currents in its ionosphere. The relative role of these mechanisms can be revealed by the flyby data and directly compared to data that was taken at Jupiter with identical instrumentation.

Faces of Pluto

NASA Image and Video Library

2015-06-11

These images, taken by NASA's New Horizons' Long Range Reconnaissance Imager (LORRI), show four different "faces" of Pluto as it rotates about its axis with a period of 6.4 days. All the images have been rotated to align Pluto's rotational axis with the vertical direction (up-down) on the figure, as depicted schematically in the upper left. From left to right, the images were taken when Pluto's central longitude was 17, 63, 130, and 243 degrees, respectively. The date of each image, the distance of the New Horizons spacecraft from Pluto, and the number of days until Pluto closest approach are all indicated in the figure.These images show dramatic variations in Pluto's surface features as it rotates. When a very large, dark region near Pluto's equator appears near the limb, it gives Pluto a distinctly, but false, non-spherical appearance. Pluto is known to be almost perfectly spherical from previous data. These images are displayed at four times the native LORRI image size, and have been processed using a method called deconvolution, which sharpens the original images to enhance features on Pluto. Deconvolution can occasionally introduce "false" details, so the finest details in these pictures will need to be confirmed by images taken from closer range in the next few weeks. All of the images are displayed using the same brightness scale. http://photojournal.jpl.nasa.gov/catalog/PIA19686

Possible occultation by Pluto from US East Coast

NASA Astrophysics Data System (ADS)

Waagen, Elizabeth O.

2012-06-01

We have been asked to help disseminate the news of a possible occultation by Pluto visible to observers on the US East coast. Although the AAVSO does not ordinarily issue announcements of upcoming occultations, in this case the object is Pluto and the NASA New Horizons mission (http://www.nasa.gov/mission_pages/newhorizons/main/index.html) will be visiting Pluto in 2015. The information below has been supplied by Dr. Leslie Young (Southwest Research Institute), who is coordinating this observing campaign on Pluto. Dr. Young is also Deputy Project Scientist for the New Horizons mission. ALERT: Possible Pluto occultation Wednesday night (2012/06/14 03:28 UT) from US East coast. CONTACT: Leslie Young (layoung@boulder.swri.edu; work: 303-546-6057; skype: drpluto). Also see our planning pages in progress at http://wiki.boulder.swri.edu/mediawiki/index.php/2012-06-14_Pluto_occultation. Pluto's thin, nitrogen atmosphere is in vapor-pressure equilibrium with the surface ice, and changes seasonally. We've seen it double since 1988, and now we measure its pressure once or twice a year. The technique we use is stellar occultation, when a star passes behind Pluto's atmosphere. The atmosphere defocuses the starlight. By the timing of the fading of the star, we measure the pressure and temperature in Pluto's atmosphere at ~10 km resolution. MORE INFORMATION: See http://wiki.boulder.swri.edu/mediawiki/index.php/2012-06-14_Pluto_occultation.

A Colorful Landing on Pluto

NASA Image and Video Library

2017-01-21

What would it be like to actually land on Pluto? This image is one of more than 100 images taken by NASA's New Horizons spacecraft over six weeks of approach and close flyby in the summer of 2015. A video offers a trip down onto the surface of Pluto -- starting with a distant view of Pluto and its largest moon, Charon -- and leading up to an eventual ride in for a "landing" on the shoreline of Pluto's informally named Sputnik Planitia. After a 9.5-year voyage covering more than three billion miles, New Horizons flew through the Pluto system on July 14, 2015, coming within 7,800 miles (12,500 kilometers) of Pluto. Carrying powerful telescopic cameras that could spot features smaller than a football field, New Horizons sent back hundreds of images of Pluto and its moons that show how dynamic and fascinating their surfaces are. Movies are available at http://photojournal.jpl.nasa.gov/catalog/PIA11709

25. INTERIOR VIEW TO THE NORTH OF ROOM 149, THE ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

25. INTERIOR VIEW TO THE NORTH OF ROOM 149, THE ENTRANCE HALLWAY TO THE POST-MORTEM CELLS IN THE HOT DISASSEMBLY AREA. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

2. VIEW TO THE SOUTHWEST OF THE MAIN EMAD BUILDING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

2. VIEW TO THE SOUTHWEST OF THE MAIN E-MAD BUILDING WITH THE COLD BAY ON THE EAST (LEFT) AND THE HOT BAY ON THE WEST (RIGHT). - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician moves a switch. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

NASA Image and Video Library

2003-08-27

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician moves a switch. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician turns on a switch. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

NASA Image and Video Library

2003-08-27

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician turns on a switch. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

Pluto: The Farthest Planet (Usually).

ERIC Educational Resources Information Center

Universe in the Classroom, 1988

1988-01-01

Provides background information about the planet Pluto. Includes the history of Pluto and discusses some of the common misconceptions about the planets. Addresses some of the recent discoveries about Pluto and contains a resource list of books, articles, and a videotape. (TW)

DOE Office of Scientific and Technical Information (OSTI.GOV)

Norris, R.S.; Arkin, W.M.

The US. nuclear stockpile is at its lowest level since late 1958 or early 1959. In the past year, many weapons were returned to central military storage depots in the United States and funneled to the Energy Department's Pantex facility for final disassembly and disposal. This article presents a table showing the author's current estimate of the composition of the current operational stockpile, which contains some 10,500 warheads. Also categorized are warheads in [open quotes]inactive reserve[close quotes] and warheads awaiting eventual disassembly. The warheads are generally grouped as bombs, submarine-launched ballistic missiles, intercontinental ballistic missiles, air-launched cruise missiles, and sea-launchedmore » cruise missiles. Initial production dates and yield are listed for the warheads.« less

The Pluto-Charon System

NASA Astrophysics Data System (ADS)

Grundy, Will

2018-05-01

Pluto orbits the Sun at a mean distance of 39 AU, with an orbital period of 248 Earth years. Its orbit is just eccentric enough to cross that of Neptune. They never collide thanks to a 2:3 mean-motion resonance: Pluto completes two orbits of the Sun for every three by Neptune. The Pluto system consists of Pluto and its large satellite Charon, plus four small satellites: Styx, Nix, Kerberos, and Hydra. Pluto and Charon are spherical bodies, with diameters of 2377 and 1212 km, respectively. They are tidally locked to one another such that each spins about its axis with the same 6.39 day period as their mutual orbit about their common barycenter. Pluto's surface is dominated by frozen volatiles nitrogen, methane, and carbon monoxide. Their vapor pressure supports an atmosphere with multiple layers of photochemical hazes. Pluto's equator is marked by a belt of dark red maculae, where the photochemical haze has accumulated over time. Some regions are ancient and cratered, while others are geologically active via processes including sublimation and condensation, glaciation, and eruption of material from the subsurface. The surfaces of the satellites are dominated by water ice. Charon has dark red polar stains produced from chemistry fed by Pluto's escaping atmosphere. The existence of a planet beyond Neptune had been postulated by Percival Lowell and William Pickering in the early 20th century, to account for supposed clustering in comet aphelia and perturbations of the orbit of Uranus. Both lines of evidence turned out to be spurious, but they motivated a series of searches that culminated in Clyde Tombaugh's discovery of Pluto in 1930, at the observatory Lowell had founded in Arizona. Over subsequent decades, basic facts about Pluto were hard-won through application of technological advances in astronomical instrumentation. The progression from photographic plates, through photoelectric photometers, to digital array detectors, space-based telescopes, and ultimately, direct exploration by robotic spacecraft each revealed more about Pluto. A key breakthrough came in 1978 with the discovery of Charon by Christy and Harrington. Charon's orbit revealed the mass of the system. Observations of stellar occultations constrained the sizes of Pluto and Charon, and enabled the detection of Pluto's atmosphere in 1988. Spectroscopic instruments revealed Pluto's volatile ices. In a series of mutual events from 1985 through 1990, Pluto and Charon alternated in passing in front of the other as seen from Earth. Observations of these events provided additional constraints on their sizes and albedo patterns and revealed their distinct compositions. Hubble Space Telescope's vantage above Earth's atmosphere enabled further mapping of Pluto's albedo patterns and the discovery of the small satellites. NASA's New Horizons spacecraft flew through the system in 2015. Its instruments mapped the diversity and compositions of geological features on Pluto and Charon and provided detailed information on Pluto's atmosphere and its interaction with the solar wind.

Pluto's Radius

NASA Astrophysics Data System (ADS)

Young, Eliot F.; Young, L. A.; Buie, M.

2007-10-01

The size of Pluto has been difficult to measure. Stellar occultations by Pluto have not yet probed altitudes lower than 1198 km, assuming the clear atmosphere model of Elliot, Person and Qu (2003). Differential refraction by Pluto's atmosphere attenuates the light from an occulted star to a level that is indistinguishable from the zero-level baseline long before Pluto's solid surface is a factor. Since Charon has no detectable atmosphere, its radius was well determined from a stellar occultation in 2005 (Gulbis et al. 2006, Sicardy et al. 2006). Combined with the mutual event photometry (Charon transited Pluto every 6.38 days between 1986 through 1992) - for which differential refraction is a negligible effect - the well-known radius of Charon translates into a more accurate radius for Pluto's solid surface. Our preliminary solid radius estimate for Pluto is 1161 km. We will discuss error bars and the correlations of this determination with Pluto albedo maps. We will also discuss the implications for Pluto's thermal profile, surface temperature and pressure, and constraints on the presence of a haze layer. This work is funded by NASA's Planetary Astronomy program. References Elliot, J.L., Person, M.J., & Qu, S. 2003, "Analysis of Stellar Occultation Data. II. Inversion, with Application to Pluto and Triton." AJ, 126, 1041. Gulbis, A.A.S. et al. 2006, "Charon's radius and atmospheric constraints from observations of a stellar occultation." Nature, 49, 48. Sicardy, B. et al. 2006, "Charon's size and an upper limit on its atmosphere from a stellar occultation." Nature, 49, 52.

Highly integrated Pluto payload system (HIPPS): a sciencecraft instrument for the Pluto mission

NASA Astrophysics Data System (ADS)

Stern, S. Alan; Slater, David C.; Gibson, William; Reitsema, Harold J.; Delamere, W. Alan; Jennings, Donald E.; Reuter, D. C.; Clarke, John T.; Porco, Carolyn C.; Shoemaker, Eugene M.; Spencer, John R.

1995-09-01

We describe the design concept for the highly integrated Pluto payload system (HIPPS): a highly integrated, low-cost, light-weight, low-power instrument payload designed to fly aboard the proposed NASA Pluto flyby spacecraft destined for the Pluto/Charon system. The HIPPS payload is designed to accomplish all of the Pluto flyby prime (IA) science objectives, except radio science, set forth by NASA's Outer Planets Science Working Group (OPSWG) and the Pluto Express Science Definition Team (SDT). HIPPS contains a complement of three instrument components within one common infrastructure; these are: (1) a visible/near UV CCD imaging camera; (2) an infrared spectrograph; and (3) an ultraviolet spectrograph. A detailed description of each instrument is presented along with how they will meet the IA science requirements.

The New Horizons Mission to Pluto and Flyby of Jupiter

NASA Technical Reports Server (NTRS)

Stern, Alan; Weaver, Hal; Young, Leslie; Bagenal, Fran; Binzel, Richard; Buratti, Bonnie; Cheng, andy; Cruikshank, Dale; Gladstone, Randy; Grundy, Will;

Global albedos of Pluto and Charon from LORRI New Horizons observations

NASA Astrophysics Data System (ADS)

Buratti, B. J.; Hofgartner, J. D.; Hicks, M. D.; Weaver, H. A.; Stern, S. A.; Momary, T.; Mosher, J. A.; Beyer, R. A.; Verbiscer, A. J.; Zangari, A. M.; Young, L. A.; Lisse, C. M.; Singer, K.; Cheng, A.; Grundy, W.; Ennico, K.; Olkin, C. B.

2017-05-01

The exploration of the Pluto-Charon system by the New Horizons spacecraft represents the first opportunity to understand the distribution of albedo and other photometric properties of the surfaces of objects in the Solar System's ;Third Zone; of distant ice-rich bodies. Images of the entire illuminated surface of Pluto and Charon obtained by the Long Range Reconnaissance Imager (LORRI) camera provide a global map of Pluto that reveals surface albedo variegations larger than any other Solar System world except for Saturn's moon Iapetus. Normal reflectances on Pluto range from 0.08-1.0, and the low-albedo areas of Pluto are darker than any region of Charon. Charon exhibits a much blander surface with normal reflectances ranging from 0.20-0.73. Pluto's albedo features are well-correlated with geologic features, although some exogenous low-albedo dust may be responsible for features seen to the west of the area informally named Tombaugh Regio. The albedo patterns of both Pluto and Charon are latitudinally organized, with the exception of Tombaugh Regio, with darker regions concentrated at the Pluto's equator and Charon's northern pole. The phase curve of Pluto is similar to that of Triton, the large moon of Neptune believed to be a captured Kuiper Belt Object (KBO), while Charon's is similar to that of the Moon. Preliminary Bond albedos are 0.25 ± 0.03 for Charon and 0.72 ± 0.07 for Pluto. Maps of an approximation to the Bond albedo for both Pluto and Charon are presented for the first time. Our work shows a connection between very high albedo (near unity) and planetary activity, a result that suggests the KBO Eris may be currently active.

30. INTERIOR VIEW TO THE NORTH OF THE WEST CORRIDOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

30. INTERIOR VIEW TO THE NORTH OF THE WEST CORRIDOR OF THE BASEMENT IN THE HOT DISASSEMBLY AREA. ELECTRIC MOTORS LINE THE WEST WALL. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Pluto' interaction with its space environment: Solar wind, energetic particles, and dust

NASA Astrophysics Data System (ADS)

Bagenal, F.; Horányi, M.; McComas, D. J.; McNutt, R. L.; Elliott, H. A.; Hill, M. E.; Brown, L. E.; Delamere, P. A.; Kollmann, P.; Krimigis, S. M.; Kusterer, M.; Lisse, C. M.; Mitchell, D. G.; Piquette, M.; Poppe, A. R.; Strobel, D. F.; Szalay, J. R.; Valek, P.; Vandegriff, J.; Weidner, S.; Zirnstein, E. J.; Stern, S. A.; Ennico, K.; Olkin, C. B.; Weaver, H. A.; Young, L. A.; Gladstone, G. R.; Grundy, W. M.; McKinnon, W. B.; Moore, J. M.; Spencer, J. R.; Andert, T.; Andrews, J.; Banks, M.; Bauer, B.; Bauman, J.; Barnouin, O. S.; Bedini, P.; Beisser, K.; Beyer, R. A.; Bhaskaran, S.; Binzel, R. P.; Birath, E.; Bird, M.; Bogan, D. J.; Bowman, A.; Bray, V. J.; Brozovic, M.; Bryan, C.; Buckley, M. R.; Buie, M. W.; Buratti, B. J.; Bushman, S. S.; Calloway, A.; Carcich, B.; Cheng, A. F.; Conard, S.; Conrad, C. A.; Cook, J. C.; Cruikshank, D. P.; Custodio, O. S.; Dalle Ore, C. M.; Deboy, C.; Dischner, Z. J. B.; Dumont, P.; Earle, A. M.; Ercol, J.; Ernst, C. M.; Finley, T.; Flanigan, S. H.; Fountain, G.; Freeze, M. J.; Greathouse, T.; Green, J. L.; Guo, Y.; Hahn, M.; Hamilton, D. P.; Hamilton, S. A.; Hanley, J.; Harch, A.; Hart, H. M.; Hersman, C. B.; Hill, A.; Hinson, D. P.; Holdridge, M. E.; Howard, A. D.; Howett, C. J. A.; Jackman, C.; Jacobson, R. A.; Jennings, D. E.; Kammer, J. A.; Kang, H. K.; Kaufmann, D. E.; Kusnierkiewicz, D.; Lauer, T. R.; Lee, J. E.; Lindstrom, K. L.; Linscott, I. R.; Lunsford, A. W.; Mallder, V. A.; Martin, N.; Mehoke, D.; Mehoke, T.; Melin, E. D.; Mutchler, M.; Nelson, D.; Nimmo, F.; Nunez, J. I.; Ocampo, A.; Owen, W. M.; Paetzold, M.; Page, B.; Parker, A. H.; Parker, J. W.; Pelletier, F.; Peterson, J.; Pinkine, N.; Porter, S. B.; Protopapa, S.; Redfern, J.; Reitsema, H. J.; Reuter, D. C.; Roberts, J. H.; Robbins, S. J.; Rogers, G.; Rose, D.; Runyon, K.; Retherford, K. D.; Ryschkewitsch, M. G.; Schenk, P.; Schindhelm, E.; Sepan, B.; Showalter, M. R.; Singer, K. N.; Soluri, M.; Stanbridge, D.; Steffl, A. J.; Stryk, T.; Summers, M. E.; Tapley, M.; Taylor, A.; Taylor, H.; Throop, H. B.; Tsang, C. C. C.; Tyler, G. L.; Umurhan, O. M.; Verbiscer, A. J.; Versteeg, M. H.; Vincent, M.; Webbert, R.; Weigle, G. E.; White, O. L.; Whittenburg, K.; Williams, B. G.; Williams, K.; Williams, S.; Woods, W. W.; Zangari, A. M.

2016-03-01

The New Horizons spacecraft carried three instruments that measured the space environment near Pluto as it flew by on 14 July 2015. The Solar Wind Around Pluto (SWAP) instrument revealed an interaction region confined sunward of Pluto to within about 6 Pluto radii. The region's surprisingly small size is consistent with a reduced atmospheric escape rate, as well as a particularly high solar wind flux. Observations from the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument suggest that ions are accelerated and/or deflected around Pluto. In the wake of the interaction region, PEPSSI observed suprathermal particle fluxes equal to about 1/10 of the flux in the interplanetary medium and increasing with distance downstream. The Venetia Burney Student Dust Counter, which measures grains with radii larger than 1.4 micrometers, detected one candidate impact in ±5 days around New Horizons' closest approach, indicating an upper limit of <4.6 kilometers-3 for the dust density in the Pluto system.

Isotopic constraints on the source of Pluto's nitrogen and the history of atmospheric escape

NASA Astrophysics Data System (ADS)

Mandt, Kathleen E.; Mousis, Olivier; Luspay-Kuti, Adrienn

2016-10-01

The origin and evolution of nitrogen in solar system bodies is an important question for understanding processes that took place during the formation of the planets and solar system bodies. Pluto has an atmosphere that is 99% molecular nitrogen, but it is unclear if this nitrogen is primordial or derived from ammonia in the protosolar nebula. The nitrogen isotope ratio is an important tracer of the origin of nitrogen on solar system bodies, and can be used at Pluto to determine the origin of its nitrogen. After evaluating the potential impact of escape and photochemistry on Pluto's nitrogen isotope ratio (14N/15N), we find that if Pluto's nitrogen originated as N2 the current ratio in Pluto's atmosphere would be greater than 324 while it would be less than 157 if the source of Pluto's nitrogen were NH3. The New Horizons spacecraft successfully visited the Pluto system in July 2015 providing a potential opportunity to measure 14N/15N in N2.

The far ultraviolet spectrum of Pluto and the discovery of its ionosphere

NASA Astrophysics Data System (ADS)

Steffl, A.; Stern, A.; Gladstone, R.; Parker, J. W.; Greathouse, T. K.; Retherford, K. D.; Young, L. A.; Schindhelm, E.; Kammer, J.; Strobel, D. F.; Summers, M. E.; Versteeg, M.; Olkin, C.; Weaver, H. A., Jr.; Hinson, D. P.; Linscott, I.

2016-12-01

During the New Horizons spacecraft's encounter with Pluto in July 2015, the Alice far ultraviolet spectrograph made numerous observations of Pluto and its atmosphere. We present here the far ultraviolet spectrum of Pluto. We observe faint emission (<0.01 Rayleighs/Ångstrom) from singly ionized nitrogen at 108.6 nm-the first detection of an ionosphere at Pluto. This N+ line is produced primarily by dissociative photoionization of molecular N2 by solar EUV photons (energy > 34.7 eV; wavelength < 36nm). Notably absent from Pluto's spectrum are emission lines from argon at 104.8 and 106.7 nm. We place upper limits on the amount of argon in Pluto's atmosphere above the tau=1 level (observed to be at 750km tangent altitude) that are significantly lower than previous models. We also identify and derive column densities for various hydrocarbon species such as C2H4 through their absorption of sunlight reflected from Pluto's surface.

Pluto's interaction with its space environment: Solar wind, energetic particles, and dust.

PubMed

Bagenal, F; Horányi, M; McComas, D J; McNutt, R L; Elliott, H A; Hill, M E; Brown, L E; Delamere, P A; Kollmann, P; Krimigis, S M; Kusterer, M; Lisse, C M; Mitchell, D G; Piquette, M; Poppe, A R; Strobel, D F; Szalay, J R; Valek, P; Vandegriff, J; Weidner, S; Zirnstein, E J; Stern, S A; Ennico, K; Olkin, C B; Weaver, H A; Young, L A

2016-03-18

The New Horizons spacecraft carried three instruments that measured the space environment near Pluto as it flew by on 14 July 2015. The Solar Wind Around Pluto (SWAP) instrument revealed an interaction region confined sunward of Pluto to within about 6 Pluto radii. The region's surprisingly small size is consistent with a reduced atmospheric escape rate, as well as a particularly high solar wind flux. Observations from the Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument suggest that ions are accelerated and/or deflected around Pluto. In the wake of the interaction region, PEPSSI observed suprathermal particle fluxes equal to about 1/10 of the flux in the interplanetary medium and increasing with distance downstream. The Venetia Burney Student Dust Counter, which measures grains with radii larger than 1.4 micrometers, detected one candidate impact in ±5 days around New Horizons' closest approach, indicating an upper limit of <4.6 kilometers(-3) for the dust density in the Pluto system. Copyright © 2016, American Association for the Advancement of Science.

Pluto and Charon in Color: Pluto-Centric View Animation

NASA Image and Video Library

2015-06-11

The first color movies from NASA's New Horizons mission show Pluto and its largest moon, Charon, and the complex orbital dance of the two bodies, known as a double planet. A near-true color movie were assembled from images made in three colors -- blue, red and near-infrared -- by the Multispectral Visible Imaging Camera on the instrument known as Ralph. The images were taken on nine different occasions from May 29-June 3, 2015. The movie is "Pluto-centric," meaning that Charon is shown as it moves in relation to Pluto, which is digitally centered in the movie. (The North Pole of Pluto is at the top.) Pluto makes one turn around its axis every 6 days, 9 hours and 17.6 minutes-the same amount of time that Charon rotates in its orbit. Looking closely at the images in this movie, one can detect a regular shift in Pluto's brightness-due to the brighter and darker terrains on its differing faces. http://photojournal.jpl.nasa.gov/catalog/PIA19689

Pluto and Charon - the dance goes on

DOE Office of Scientific and Technical Information (OSTI.GOV)

Beatty, J.K.

1987-09-01

Various methods for estimating the diameters of Pluto and Charon are discussed. The application of speckle interferometry, the timing of occultations, and the monitoring of Charon and Pluto rotations to calculate the diameter of the planet and its satellite are described. Walker (1980) estimated Charon's diameter as greater than 1200 km using the occultated star method; the speckle interferometry estimates of Baier and Weigelt (1983) are between 2710-3460 km for Pluto and between 1050-1520 km for Charon; and using the mutual events method Dunbar and Tedesco (1986) estimated the diameter of Pluto as 2300 + or - 100 km andmore » of Charon as 1500 + or - 100 km. The use of IRAS data combined with visual brightness to estimate planet and satellite diameters is examined; Tedesco et al. (1987) estimated Pluto's diameter as 2200 + or - 150 km and Charon's as 1300 + or - 150 km, and Aumann and Walker (1987) obtained estimates of 2360 km for Pluto and 1534 km for Charon. The compositions of Pluto's and Charon's atmospheres are analyzed.« less

Exploration at the Edge of the Solar System: The Pluto-Kuiper Express Mission (Invited)

NASA Astrophysics Data System (ADS)

Terrile, R. J.

1999-09-01

The Pluto-Kuiper Express mission is one component of the Outer Planets/Solar Probe Project which is part of the exploration strategy laid out in the Solar System Exploration Roadmap. The first three missions of this project are the Europa Orbiter, Pluto-Kuiper Express and the Solar Probe. All require challenging new technologies and the ability to operate in deep space and at Jupiter. Use of common management and design approaches, avionics, and mission software is planned to reduce the costs of the three missions. The Pluto-Kuiper Express mission is planned to launch in 2004 and is designed to provide the first reconnaissance of the Solar System's most distant planet, Pluto, and it, moon Charon. A gravity assist from Jupiter will allow an 8-year flight time to Pluto and the possibility of encountering one or more Edgeworth-Kuiper Belt objects after the Pluto encounter. The primary science objectives for the mission include characterizing the global geology and geomorphology of Pluto and Charon, mapping their surface composition and characterizing Pluto's neutral atmosphere and its escape rate. This mission is currently soliciting scientific investigations through a NASA Announcement of Opportunity.

Implications of the observed Pluto-Charon density contrast

NASA Astrophysics Data System (ADS)

Bierson, C. J.; Nimmo, F.; McKinnon, W. B.

2018-07-01

Observations by the New Horizons spacecraft have determined that Pluto has a larger bulk density than Charon by 153 ± 44 kg m-3 (2σ uncertainty). We use a thermal model of Pluto and Charon to determine if this density contrast could be due to porosity variations alone, with Pluto and Charon having the same bulk composition. We find that Charon can preserve a larger porous ice layer than Pluto due to its lower gravity and lower heat flux but that the density contrast can only be explained if the initial ice porosity is ≳ 30%, extends to ≳100 km depth and Pluto retains a subsurface ocean today. We also find that other processes such as a modern ocean on Pluto, self-compression, water-rock interactions, and volatile (e.g., CO) loss cannot, even in combination, explain this difference in density. Although an initially high porosity cannot be completely ruled out, we conclude that it is more probable that Pluto and Charon have different bulk compositions. This difference could arise either from forming Charon via a giant impact, or via preferential loss of H2O on Pluto due to heating during rapid accretion.

Pluto Seen from Saturn

NASA Image and Video Library

2015-07-16

As one NASA spacecraft sailed past the distant ice world of Pluto, collecting never-before-seen vistas and invaluable science data, another spacecraft turned its gaze in that direction from its outpost at Saturn. NASA's Cassini spacecraft took a momentary break from its duties to capture this far-off portrait around the time of the New Horizons encounter with Pluto. The image was taken within a few minutes of New Horizons' closest approach to Pluto. After New Horizons, Cassini was the closest spacecraft to Pluto at the time of the flyby. Pluto is the bright dot closest to the center of the field of stars seen in this view. A labeled version of the image, indicating Pluto's position, is also presented here. The four stars identified in the labeled view have visual magnitudes between about 11 and 12. The entire Pluto system -- the dwarf planet and all of its moons -- is below the resolution of this image, thus the small bright specks near the main dot representing Pluto are likely noise (possibly due to what astronomers call the point-spread function). Charon and the other moons would not be resolved at this scale. The image was obtained using the Cassini spacecraft narrow-angle camera on July 14, 2015 at a distance of about 2.4 billion miles (3.9 billion kilometers) from Pluto. http://photojournal.jpl.nasa.gov/catalog/PIA19641

Pluto's Extended Atmosphere: New Horizons Alice Lyman-α Imaging

NASA Astrophysics Data System (ADS)

Retherford, Kurt D.; Gladstone, G. Randall; Stern, S. Alan; Weaver, Harold A.; Young, Leslie A.; Ennico, Kimberly A.; Olkin, Cathy B.; Cheng, Andy F.; Greathouse, Thomas K.; Hinson, David P.; Kammer, Joshua A.; Linscott, Ivan R.; Parker, Alex H.; Parker, Joel Wm.; Pryor, Wayne R.; Schindhelm, Eric; Singer, Kelsi N.; Steffl, Andrew J.; Strobel, Darrell F.; Summers, Michael E.; Tsang, Constantine C. C.; Tyler, G. Len; Versteeg, Maarten H.; Woods, William W.; Cunningham, Nathaniel J.; Curdt, Werner

2015-11-01

Pluto's upper atmosphere is expected to extend several planetary radii, proportionally more so than for any planet in our solar system. Atomic hydrogen is readily produced at lower altitudes due to photolysis of methane and transported upward to become an important constituent. The Interplanetary Medium (IPM) provides a natural light source with which to study Pluto's atomic hydrogen atmosphere. While direct solar Lyman-α emissions dominate the signal at 121.6 nm at classical solar system distances, the contribution of diffuse illumination by IPM Lyman-α sky-glow is roughly on par at Pluto (Gladstone et al., Icarus, 2015). Hydrogen atoms in Pluto's upper atmosphere scatter these bright Lyα emission lines, and detailed simulations of the radiative transfer for these photons indicate that Pluto would appear dark against the IPM Lyα background. The Pluto-Alice UV imaging spectrograph on New Horizons conducted several observations of Pluto during the encounter to search for airglow emissions, characterize its UV reflectance spectra, and to measure the radial distribution of IPM Lyα near the disk. Our early results suggest that these model predictions for the darkening of IPM Lyα with decreasing altitude being measureable by Pluto-Alice were correct. We'll report our progress toward extracting H and CH4 density profiles in Pluto's upper atmosphere through comparisons of these data with detailed radiative transfer modeling. These New Horizons findings will have important implications for determining the extent of Pluto's atmosphere and related constraints to high-altitude vertical temperature structure and atmospheric escape.This work was supported by NASA's New Horizons project.

4. VIEW TO THE NORTHWEST OF THE COLD BAY ON ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

4. VIEW TO THE NORTHWEST OF THE COLD BAY ON THE NORTH (RIGHT) AND THE POST-MORTEM CELLS ON THE SOUTH (LEFT). ALSO ILLUSTRATED ARE THE DIFFERENT ROOF HEIGHTS OF THE BUILDING. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

5. EXTERIOR VIEW TO THE SOUTHEAST OF THE NORTH AND ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

5. EXTERIOR VIEW TO THE SOUTHEAST OF THE NORTH AND WEST ELEVATIONS, WITH THE COLD ASSEMBLY AREA TO THE RIGHT AND THE HOT DISASSEMBLY AREA TO THE LEFT. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

3. NORTH ELEVATION OF THE HOT BAY, SHOWING RAILROAD TRACKS ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

3. NORTH ELEVATION OF THE HOT BAY, SHOWING RAILROAD TRACKS LEADING TO THE MASSIVE STEEL-LINED CONCRETE ENTRANCE DOOR. PART OF THE INTRICATE HVAC SYSTEM IS WEST (RIGHT) OF THE DOOR. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

Flying Past Pluto Animation

NASA Image and Video Library

2015-08-28

This dramatic view of the Pluto system is as NASA's New Horizons spacecraft saw it in July 2015. The animation, made with real images taken by New Horizons, begins with Pluto flying in for its close-up on July 14; we then pass behind Pluto and see the atmosphere glow in sunlight before the sun passes behind Pluto's largest moon, Charon. The movie ends with New Horizons' departure, looking back on each body as thin crescents. http://photojournal.jpl.nasa.gov/catalog/PIA19873

Pluto-Charon solar wind interaction dynamics

NASA Astrophysics Data System (ADS)

Hale, J. P. M.; Paty, C. S.

2017-05-01

This work studies Charon's effects on the Pluto-solar wind interaction using a multifluid MHD model which simulates the interactions of Pluto and Charon with the solar wind as well as with each other. Specifically, it investigates the ionospheric dynamics of a two body system in which either one or both bodies possess an ionosphere. Configurations in which Charon is directly upstream and directly downstream of Pluto are considered. Depending on ionospheric and solar wind conditions, Charon could periodically pass into the solar wind flow upstream of Pluto. The results of this study demonstrate that in these circumstances Charon modifies the upstream flow, both in the case in which Charon possesses an ionosphere, and in the case in which Charon is without an ionosphere. This modification amounts to a change in the gross structure of the interaction region when Charon possesses an ionosphere but is more localized when Charon lacks an ionosphere. Furthermore, evidence is shown that supports Charon acting to partially shield Pluto from the solar wind when it is upstream of Pluto, resulting in a decrease in ionospheric loss by Pluto.

Pluto Haze

NASA Image and Video Library

2015-09-10

Two different versions of an image of Pluto's haze layers, taken by New Horizons as it looked back at Pluto's dark side nearly 16 hours after close approach, from a distance of 480,000 miles (770,000 kilometers), at a phase angle of 166 degrees. Pluto's north is at the top, and the sun illuminates Pluto from the upper right. These images are much higher quality than the digitally compressed images of Pluto's haze downlinked and released shortly after the July 14 encounter, and allow many new details to be seen. The left version has had only minor processing, while the right version has been specially processed to reveal a large number of discrete haze layers in the atmosphere. In the left version, faint surface details on the narrow sunlit crescent are seen through the haze in the upper right of Pluto's disk, and subtle parallel streaks in the haze may be crepuscular rays- shadows cast on the haze by topography such as mountain ranges on Pluto, similar to the rays sometimes seen in the sky after the sun sets behind mountains on Earth. http://photojournal.jpl.nasa.gov/catalog/PIA19880

Asbestos exposure from gaskets during disassembly of a medium duty diesel engine.

PubMed

Liukonen, Larry R; Weir, Francis W

2005-03-01

Diesel engines have historically used asbestos-containing gaskets leading to concerns of fiber release and mechanic exposure. Other published studies regarding asbestos fiber release during gasket removal have reported on short-duration events; were conducted under simulated work conditions; or had other limitations. There are no comprehensive studies relating to diesel engine gaskets under conditions similar to those reported herein, evaluating asbestos fiber release from gaskets during all facets of a complete disassembly and cleaning of a medium duty diesel engine in a busy repair and service shop by a journeyman mechanic. Asbestos content of all gaskets was identified; all disassembly tasks were described and timed; and personal and area air monitoring was conducted for each task. Twenty seven of thirty three gaskets contained chrysotile asbestos in concentrations that ranged from 5 to 70%. All but one air monitoring sample reported results below the limit of reliable detection even though plumes of visible dust were evident during various removal, cleaning, and buffing procedures. The detection limit for airborne asbestos fibers in this investigation was influenced by the presence of other shop dust in the air. Our investigation demonstrates that using shop-standard procedures in an established repair facility, a journeyman mechanic has very little potential for exposure to airborne asbestos fibers during disassembly of an engine, approximately 10% or less than that currently considered to be acceptable by OSHA.

Pluto's Ultraviolet Airglow and Detection of Ions in the Upper Atmosphere

NASA Astrophysics Data System (ADS)

Steffl, A.; Young, L. A.; Kammer, J.; Gladstone, R.; Hinson, D. P.; Summers, M. E.; Strobel, D. F.; Stern, S. A.; Weaver, H. A., Jr.; Olkin, C.; Ennico Smith, K.

2017-12-01

In July 2015, the Alice ultraviolet spectrograph aboard the New Horizons spacecraft made numerous observations of Pluto and its atmosphere. We present here the far ultraviolet reflectance spectrum of Pluto and airglow emissions from its atmosphere. At wavelengths greater than 1400Å, Pluto's spectrum is dominated by sunlight reflected from the surface of the planet. Various hydrocarbon species such as C2H4 are detected in absorption of the solar continuum. Below 1400Å, Pluto's atmosphere is opaque and the surface cannot be detected. However, after carefully removing various sources of background light, we see extremely faint airglow emissions (<0.05 Rayleighs/Ångstrom) from Pluto's atmosphere. All of the emissions are produced by nitrogen in various forms: molecular, atomic, and singly ionized. The detection of N+ at 1086Å is the first, and thus far only, direct detection of ions in Pluto's atmosphere. This N+ emission line is produced primarily by dissociative photoionization of molecular N2 by solar EUV photons (energy > 34.7 eV; wavelength < 360Å). Notably absent from Pluto's spectrum are emission lines from argon at 1048 and 1067Å. We place upper limits on the amount of argon in Pluto's atmosphere above the tau=1 level (observed to be at 750km tangent altitude) that are significantly lower than pre-encounter atmospheric models.

Disassemblability modeling technology of configurable product based on disassembly constraint relation weighted design structure matrix(DSM)

NASA Astrophysics Data System (ADS)

Qiu, Lemiao; Liu, Xiaojian; Zhang, Shuyou; Sun, Liangfeng

2014-05-01

The current research of configurable product disassemblability focuses on disassemblability evaluation and disassembly sequence planning. Little work has been done on quantitative analysis of configurable product disassemblability. The disassemblability modeling technology for configurable product based on disassembly constraint relation weighted design structure matrix (DSM) is proposed. Major factors affecting the disassemblability of configurable product are analyzed, and the disassembling degrees between components in configurable product are obtained by calculating disassembly entropies such as joint type, joint quantity, disassembly path, disassembly accessibility and material compatibility. The disassembly constraint relation weighted DSM of configurable product is constructed and configuration modules are formed by matrix decomposition and tearing operations. The disassembly constraint relation in configuration modules is strong coupling, and the disassembly constraint relation between modules is weak coupling, and the disassemblability configuration model is constructed based on configuration module. Finally, taking a hydraulic forging press as an example, the decomposed weak coupling components are used as configuration modules alone, components with a strong coupling are aggregated into configuration modules, and the disassembly sequence of components inside configuration modules is optimized by tearing operation. A disassemblability configuration model of the hydraulic forging press is constructed. By researching the disassemblability modeling technology of product configuration design based on disassembly constraint relation weighted DSM, the disassembly property in maintenance, recycling and reuse of configurable product are optimized.

The Cosmochemistry of Pluto: A Primordial Origin of Volatiles?

NASA Astrophysics Data System (ADS)

Glein, C. R.; Waite, J. H., Jr.

2017-12-01

Pluto is a wonderland of volatiles. Nitrogen, methane, and carbon monoxide are the principal volatiles that maintain its tenuous atmosphere, and they have also created a mesmerizing landscape of icy geological features, including Pluto's iconic "heart". Recent data, particularly those returned by the New Horizons mission [1-3], allow us to begin testing hypotheses for the cosmochemical origins of these world-shaping species on Pluto. Here, we investigate if Pluto's volatiles could have been accreted in its building blocks. We take both bottom-up and top-down approaches in testing this hypothesis in terms of mass balance. We estimate Pluto's primordial inventory of volatiles by scaling a range of cometary abundances up to the ice mass fraction of Pluto. We also make estimates of the present and lost inventories of volatiles based on surface observations and interpretations, as well as different scenarios of atmospheric photochemistry and escape. We find that, if primordial Pluto resembled a giant comet with respect to volatile abundances, then the initial volatile inventory would have been sufficient to account for the estimated present and lost inventories. This consistency supports a primordial origin for Pluto's volatiles. However, the observed ratio of CO/N2 in Pluto's atmosphere [4] is several orders of magnitude lower than the nominal cometary value. We are currently using phase equilibrium and rate models to explore if volatile layering in Sputnik Planitia, or the destruction of CO in a past or present subsurface ocean of liquid water could explain the apparent depletion of CO on Pluto. References: [1] Moore et al. (2016) Science 351, 1284. [2] Grundy et al. (2016) Science 351, aad9189. [3] Gladstone et al. (2016) Science 351, aad8866. [4] Lellouch et al. (2017) Icarus 286, 289.

Pluto and Charon: A Case of Precession-Orbit Resonance?

NASA Technical Reports Server (NTRS)

Rubincam, David Parry; Smith, David E. (Technical Monitor)

2000-01-01

Pluto may be the only known case of precession-orbit resonance in the solar system. The Pluto-Charon system orbits the Sun with a period of 1 Plutonian year, which is 250.8 Earth years. The observed parameters of the system are such that Charon may cause Pluto to precess with a period near 250.8 Earth years. This gives rise to two possible resonances, heretofore unrecognized. The first is due to Pluto's orbit being highly eccentric, giving solar torques on Charon with a period of 1 Plutonian year. Charon in turn drives Pluto near its precession period. Volatiles, which are expected to shuttle across Pluto's surface between equator and pole as Pluto's obliquity oscillates, might change the planet's dynamical flattening enough so that Pluto crosses the nearby resonance, forcing the planet's equatorial plane to depart from Charon's orbital plane. The mutual tilt can reach as much as 2 deg after integrating over 5.6 x 10(exp 6) years, depending upon how close Pluto is to the resonance and the supply of volatiles. The second resonance is due to the Sun's traveling above and below Charon's orbital plane; it has a period half that of the eccentricity resonance. Reaching this half-Plutonian year resonance requires a much larger but still theoretically possible amount of volatiles. In this case the departure of Charon from an equatorial orbit is about 1 deg after integrating for 5.6 x 10(exp 6) years. The calculations ignore libration and tidal friction. It is not presently known how large the mutual tilt can grow over the age of the solar system, but if it remains only a few degrees, then observing such small angles from a Pluto flyby mission would be difficult. It is not clear why the parameters of the Pluto-Charon system are so close to the eccentricity resonance.

Secrets Revealed from Pluto Twilight Zone

NASA Image and Video Library

2016-06-02

NASA's New Horizons spacecraft took this stunning image of Pluto only a few minutes after closest approach on July 14, 2015. The image was obtained at a high phase angle -- that is, with the sun on the other side of Pluto, as viewed by New Horizons. Seen here, sunlight filters through and illuminates Pluto's complex atmospheric haze layers. The southern portions of the nitrogen ice plains informally named Sputnik Planum, as well as mountains of the informally named Norgay Montes, can also be seen across Pluto's crescent at the top of the image. Looking back at Pluto with images like this gives New Horizons scientists information about Pluto's hazes and surface properties that they can't get from images taken on approach. The image was obtained by New Horizons' Ralph/Multispectral Visual Imaging Camera (MVIC) approximately 13,400 miles (21,550 kilometers) from Pluto, about 19 minutes after New Horizons' closest approach. The image has a resolution of 1,400 feet (430 meters) per pixel. Pluto's diameter is 1,475 miles (2,374 kilometers). The inset at top right in the annotated version shows a detail of Pluto's crescent, including an intriguing bright wisp (near the center) measuring tens of miles across that may be a discreet, low-lying cloud in Pluto's atmosphere; if so, it would be the only one yet identified in New Horizons imagery. This cloud -- if that's what it is -- is visible for the same reason the haze layers are so bright: illumination from the sunlight grazing Pluto's surface at a low angle. Atmospheric models suggest that methane clouds can occasionally form in Pluto's atmosphere. The scene in this inset is 140 miles (230 kilometers) across. The inset at bottom right shows more detail on the night side of Pluto. This terrain can be seen because it is illuminated from behind by hazes that silhouette the of the annotated version limb. The topography here appears quite rugged, and broad valleys and sharp peaks with relief totaling 3 miles (5 kilometers) are apparent. This image, made from closer range, is much better than the lower-resolution images of this same terrain taken several days before closest approach. These silhouetted terrains therefore act as a useful "anchor point," giving New Horizons scientists a rare, detailed glimpse at the lay of the land in this mysterious part of Pluto seen at high resolution only in twilight. The scene in this inset is 460 miles (750 kilometers) wide. http://photojournal.jpl.nasa.gov/catalog/PIA20727

Disassembly Control of Saccharide-Based Amphiphiles Driven by Electrostatic Repulsion.

PubMed

Yamada, Taihei; Kokado, Kenta; Sada, Kazuki

2017-03-14

According to the design of disassembly using electrostatic repulsion, novel amphiphiles consisting of a lipophilic ion part and a hydrophilic saccharide part were synthesized via the facile copper-catalyzed click reaction, and their molecular assemblies in water and chloroform were studied. The amphiphiles exhibited a molecular orientation opposite to that of the conventional amphiphiles in each case. ζ Potential measurements indicated that the lipophilic ion part is exposed outside in chloroform. The size of a solvophobic part in the amphiphiles dominates the size of an assembling structure; that is, in water, these amphiphiles tethering different lengths of the saccharide part exhibited almost identical assembling size, whereas in chloroform, the size depends on the length of the saccharide part in the amphiphiles.

Clues From Pluto's Ions

NASA Astrophysics Data System (ADS)

Kohler, Susanna

2016-05-01

Nearly a year ago, in July 2015, the New Horizons spacecraft passed by the Pluto system. The wealth of data amassed from that flyby is still being analyzed including data from the Solar Wind Around Pluto (SWAP) instrument. Recent examination of this data has revealedinteresting new information about Plutos atmosphere and how the solar wind interacts with it.A Heavy Ion TailThe solar wind is a constant stream of charged particles released by the Sun at speeds of around 400 km/s (thats 1 million mph!). This wind travels out to the far reaches of the solar system, interacting with the bodies it encounters along the way.By modeling the SWAP detections, the authors determine the directions of the IMF that could produce the heavy ions detected. Red pixels represent IMF directions permitted. No possible IMF could reproduce the detections if the ions are nitrogen (bottom panels), and only retrograde IMF directions can produce the detections if the ions are methane. [Adapted from Zirnstein et al. 2016]New Horizons data has revealed that Plutos atmosphere leaks neutral nitrogen, methane, and carbon monoxide molecules that sometimes escape its weak gravitational pull. These molecules become ionized and are subsequently picked up by the passing solar wind, forming a tail of heavy ions behind Pluto. The details of the geometry and composition of this tail, however, had not yet been determined.Escaping MethaneIn a recent study led by Eric Zirnstein (Southwest Research Institute), the latest analysis of data from the SWAP instrument on board New Horizons is reported. The team used SWAPs ion detections from just after New Horizons closest approach to Pluto to better understand how the heavy ions around Pluto behave, and how the solar wind interacts with Plutos atmosphere.In the process of analyzing the SWAP data, Zirnstein and collaborators first establish what the majority of the heavy ions picked up by the solar wind are. Models of the SWAP detections indicate they are unlikely to be nitrogen ions, despite nitrogen being the most abundant molecule in Plutos atmosphere. Instead, the detections are likely of methane ions possibly present because methane molecules are lighter, allowing them to more efficiently escape Plutos atmosphere.Reconstructed origins of heavy ions detected by SWAP shortly after New Horizons closest approach to Pluto. Color represents the energy at the time of detection. [Adapted from Zirnstein et al. 2016]Magnetic DirectionNew Horizons does not have a magnetometer on board, which prevented it from making direct measurements of the interplanetary magnetic field (IMF; the solar magnetic field extended throughout the solar system) during the Pluto encounter. In spite of this, Zirnstein and collaborators are able to determine the IMF direction using some clever calculations about SWAPs field of view and the energies of heavy ions it detected.They demonstrate that the IMF was likely oriented roughly parallel to the ecliptic plane, and in the opposite direction of Plutos orbital motion, during New Horizons Pluto encounter. This would cause the solar wind to deflect southward around Pluto, resulting in a north-south asymmetry in the heavy ion tail behind Pluto.The new knowledge gained from SWAP about the geometry and the composition of Plutos extended atmosphere will help us to interpret further data from New Horizons. Ultimately, this provides us with a better understanding both of Plutos atmosphere and how the solar wind interacts with bodies in our solar system.CitationE. J. Zirnstein et al 2016 ApJ 823 L30. doi:10.3847/2041-8205/823/2/L30

Approaching the new reality. [changes in NASA space programs due to US economy

NASA Technical Reports Server (NTRS)

Diaz, Al V.

1993-01-01

The focus on more frequent access to space through smaller, less costly missions, and on NASA's role as a source of technological advance within the U.S. economy is discussed. The Pluto fast flyby mission is examined as an illustration of this approach. Testbeds are to be developed to survive individual programs, becoming permanent facilities, to allow for technological upgrades on an ongoing basis.

Pluto Express: Mission to Pluto

NASA Technical Reports Server (NTRS)

Giuliano, J. A.

1996-01-01

Pluto is the smallest, outermost and last-discovered planet in the Solar System and the only one that has never been visited by a spacecraft from Earth. Pluto and its relatively large satellite Charon are the destinations of a proposed spacecraft mission for the next decade, being developed for NASA by scientists and engineers at NASA's Jet Propulsion Laboratory.

"Pluto Has Been a Planet My Whole Life!" Emotions, Attitudes, and Conceptual Change in Elementary Students' Learning about Pluto's Reclassification

ERIC Educational Resources Information Center

Broughton, Suzanne H.; Sinatra, Gale M.; Nussbaum, E. Michael

2013-01-01

Learning about certain scientific topics has potential to spark strong emotions among students. We investigated whether emotions predicted students' attitudes after engaging in independent rereading and/or rereading plus discussion about Pluto's reclassification. Fifth and sixth grade students read a refutation text on Pluto's reclassification.…

Methane in Pluto's Atmosphere

NASA Astrophysics Data System (ADS)

Roe, Henry G.

2006-09-01

The abundance of methane in Pluto's atmosphere has not been remeasured since its initial detection in 1992 by Young et al. (1997). As Pluto recedes from the Sun its atmosphere should eventually collapse and freeze out on the surface, but recent occultation observations (Elliot et al. 2003) show an expansion of the atmosphere rather than contraction. New measurements of Pluto's atmospheric methane abundance are warranted. We obtained high resolution (R=25000) near-infrared spectra of Pluto in July 2006 with NIRSPEC at the W.M. Keck II telescope and will report our initial analysis and results.

Global Mosaics of Pluto and Charon

NASA Image and Video Library

2017-07-14

Global mosaics of Pluto and Charon projected at 300 meters (985 feet) per pixel that have been assembled from most of the highest resolution images obtained by the Long-Range Reconnaissance Imager (LORRI) and the Multispectral Visible Imaging Camera (MVIC) onboard New Horizons. Transparent, colorized stereo topography data generated for the encounter hemispheres of Pluto and Charon have been overlain on the mosaics. Terrain south of about 30°S on Pluto and Charon was in darkness leading up to and during the flyby, so is shown in black. "S" and "T" respectively indicate Sputnik Planitia and Tartarus Dorsa on Pluto, and "C" indicates Caleuche Chasma on Charon. All feature names on Pluto and Charon are informal. https://photojournal.jpl.nasa.gov/catalog/PIA21862

Improved orbital and physical parameters for the Pluto-Charon system

NASA Astrophysics Data System (ADS)

Tholen, D. J.; Buie, M. W.; Binzel, R. P.; Frueh, M. L.

1987-07-01

Analysis of the observations of several Pluto-Charon occultation and transit events in 1985 and 1986 has provided a more detailed knowledge of the system. The sum of the radii of Pluto and Charon is 1786±19 kilometers, but the individual radii are somewhat more poorly determined; Pluto is 1145±46 kilometers in radius and Charon is 642±34 kilometers in radius. The mean density of the system is 1.84±0.19 grams per cubic centimeter implying that more than half of the mass is due to rock. Charon appears to have hemispheres of two different colors, the Pluto-facing side being neutral in color and the opposite hemisphere being a reddish color similar to Pluto.

Sedna Size Comparisons Artist Concept

NASA Image and Video Library

2004-03-15

The artist's rendition shows the newly discovered planet-like object, dubbed "Sedna," in relation to other bodies in the solar system, including Earth and its Moon; Pluto; and Quaoar, a planetoid beyond Pluto that was until now the largest known object beyond Pluto. The diameter of Sedna is slightly smaller than Pluto's but likely somewhat larger than Quaoar. http://photojournal.jpl.nasa.gov/catalog/PIA05567

Past epochs of significantly higher pressure atmospheres on Pluto

NASA Astrophysics Data System (ADS)

Stern, S. A.; Binzel, R. P.; Earle, A. M.; Singer, K. N.; Young, L. A.; Weaver, H. A.; Olkin, C. B.; Ennico, K.; Moore, J. M.; McKinnon, W. B.; Spencer, J. R.; New Horizons Geology; Geophysics; Atmospheres Teams

2017-05-01

Pluto is known to have undergone thousands of cycles of obliquity change and polar precession. These variations have a large and corresponding impact on the total average solar insolation reaching various places on Pluto's surface as a function of time. Such changes could produce dramatic increases in surface pressure and may explain certain features observed by New Horizons on Pluto's surface, including some that indicate the possibility of surface paleo-liquids. This paper is the first to discuss multiple lines of geomorphological evidence consistent with higher pressure epochs in Pluto's geologic past, and it also the first to provide a mechanism for potentially producing the requisite high pressure conditions needed for an environment that could support liquids on Pluto. The presence of such liquids and such conditions, if borne out by future work, would fundamentally affect our view of Pluto's past climate, volatile transport, and geological evolution. This paper motivates future, more detailed climate modeling and geologic interpretation efforts in this area.

31. INTERIOR VIEW TO THE EAST OF THE FIRST FLOOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

31. INTERIOR VIEW TO THE EAST OF THE FIRST FLOOR SOUTH CORRIDOR AND VIEWING GALLERY TO THE DISASSEMBLY BAY AND POST-MORTEM CELLS. VIEWING STATIONS ARE ON BOTH SIDES OF THE CORRIDOR. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

38. INTERIOR VIEW TO THE NORTHWEST OF THE SECOND FLOOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

38. INTERIOR VIEW TO THE NORTHWEST OF THE SECOND FLOOR CORRIDOR ON THE SOUTH SIDE OF THE DISASSEMBLY BAY. VIEWING AND WORK STATIONS ARE ALONG THE NORTH WALL OF THE CORRIDOR. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

6. INTERIOR VIEW TO THE EAST OF SOUTHEAST CORNER OF ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

6. INTERIOR VIEW TO THE EAST OF SOUTHEAST CORNER OF THE HOT BAY. A LARGE MANIPULATOR ARM AND HORIZONTAL TRACKING SYSTEM IS SHOWN ABOVE SMALLER MANIPULATOR ARM WORK STATIONS. ASSOCIATED WITH THE WORK STATIONS ARE OBSERVATION WINDOWS. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician (left) looks at the circuit breaker lights in the cabin. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

NASA Image and Video Library

2003-08-27

KENNEDY SPACE CENTER, FLA. - During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician (left) looks at the circuit breaker lights in the cabin. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

New Horizons Sees Pluto (Sept. 24) Note: There is debate within the science community as to whether

NASA Technical Reports Server (NTRS)

2007-01-01

A white arrow marks Pluto in this New Horizons Long Range Reconnaissance Imager (LORRI) picture taken Sept. 21, 2006. Seen at a distance of about 4.2 billion kilometers (2.6 billion miles) from the spacecraft, Pluto is little more than a faint point of light among a dense field of stars. Mission scientists knew they had Pluto in their sights when LORRI detected an unresolved 'point' in Pluto's predicted position, moving at the planet's expected motion across the constellation of Sagittarius near the plane of the Milky Way galaxy.

New Horizons Sees Pluto (Sept. 21) Note: There is debate within the science community as to whether

NASA Technical Reports Server (NTRS)

2007-01-01

A white arrow marks Pluto in this New Horizons Long Range Reconnaissance Imager (LORRI) picture taken Sept. 21, 2006. Seen at a distance of about 4.2 billion kilometers (2.6 billion miles) from the spacecraft, Pluto is little more than a faint point of light among a dense field of stars. Mission scientists knew they had Pluto in their sights when LORRI detected an unresolved 'point' in Pluto's predicted position, moving at the planet's expected motion across the constellation of Sagittarius near the plane of the Milky Way galaxy.

Pluto: A Global Perspective

NASA Image and Video Library

2016-05-02

NASA New Horizons mission science team has produced this updated panchromatic black-and-white global map of Pluto. The map includes all resolved images of Pluto surface acquired between July 7-14, 2015.

Is Pluto a planet? Student powered video rap ';battle' over tiny Pluto's embattled planetary standing

NASA Astrophysics Data System (ADS)

Beisser, K.; Cruikshank, D. P.; McFadden, T.

2013-12-01

Is Pluto a planet? Some creative low income Bay-area middle-schoolers put a musical spin on this hot science debate with a video rap ';battle' over tiny Pluto's embattled planetary standing. The students' timing was perfect, with NASA's New Horizons mission set to conduct the first reconnaissance of Pluto and its moons in July 2015. Pluto - the last of the nine original planets to be explored by spacecraft - has been the subject of scientific study and speculation since Clyde Tombaugh discovered it in 1930, orbiting the Sun far beyond Neptune. Produced by the students and a very creative educator, the video features students 'battling' back and forth over the idea of Pluto being a planet. The group collaborated with actual space scientists to gather information and shot their video before a 'green screen' that was eventually filled with animations and visuals supplied by the New Horizons mission team. The video debuted at the Pluto Science Conference in Maryland in July 2013 - to a rousing response from researchers in attendance. The video marks a nontraditional approach to the ongoing 'great planet debate' while educating viewers on a recently discovered region of the solar system. By the 1990s, researchers had learned that Pluto possessed multiple exotic ices on its surface, a complex atmosphere and seasonal cycles, and a large moon (Charon) that likely resulted from a giant impact on Pluto itself. It also became clear that Pluto was no misfit among the planets - as had long been thought - but the largest and brightest body in a newly discovered 'third zone' of our planetary system called the Kuiper Belt. More recent observations have revealed that Pluto has a rich system of satellites - five known moons - and a surface that changes over time. Scientists even speculate that Pluto may possess an internal ocean. For these and other reasons, the 2003 Planetary Decadal Survey ranked a Pluto/Kuiper Belt mission as the highest priority mission for NASA's newly created New Frontiers program - and that mission is New Horizons. This effort was funded by a Hewlett Packard Sustainability and Social Innovation grant, the Silicon Valley Education Foundation and a Kickstarter campaign to expand this effort to multiple schools. This process and product are great examples of teamwork between scientists and science educators - and show how we can use the appeal of video to communicate science to diverse audiences.

Pluto's elongated dark regions formed by the Charon-forming giant impact

NASA Astrophysics Data System (ADS)

Genda, Hidenori; Sekine, Yusuhito; Kamata, Shunichi; Funatsu, Taro

2017-04-01

The New Horizons spacecraft has found elongated dark areas in the equatorial region of Pluto, which were informally called "the Whale" or Cthulhu Region (Stern et al. 2015). Here we examine the possibility that the dark areas on Pluto were formed by thermal alterations and polymerization of interstellar volatiles caused by a Charon-forming giant impact. Pluto is one of the largest Kuiper belt objects, which is highly likely to contain various interstellar volatiles, including aldehyde and ammonia. The previous study (Cordy et al. 2011) shows that these interstellar volatiles are thermally polymerized in solutions at high temperatures, forming complex insoluble organic solids. Given the satellite-to-planet mass ratio, the Pluto-Charon system is suggested to be of a giant impact origin (Canup 2005). Impact-induced heating on Pluto could have converted these volatile into complex organic matter in solution near the surface, which may explain the presence of dark areas in the equatorial region of Pluto. Here, we produce complex organic matter for various temperatures by thermal polymerization of formaldehyde and ammonia in solutions. By measuring the UV-VIS absorption spectra of the produced organic matter, we found that the color of the solution changes to be dark if the temerature is above 50 degree C for months or more. This duration corresponds to the cooling timescale of a water pond with 500-km thickness. By using SPH code (Genda et al. 2015), we carried out many simulations of a giant impact, and we found that a molten hot pond with > 500-km thickness is formed around the equatorial region of Pluto by a Charon-forming giant impact, if the water/rock mixing mass ratio is less than 1 or if the pre-impact interior temperature is 150 K. Both the dark equatorial region and a Charon-sized moon are formed when the pre-impact Pluto is undifferentiated. To keep a rock-rich Pluto undifferentiated at time of the giant impact, Pluto may have been formed >100 Myrs after CAIs, and the giant impact may have occurred <100 Myrs after the Pluto's formation.

Seasonal Nitrogen Cycles on Pluto

NASA Technical Reports Server (NTRS)

Hansen, Candice J.; Paige, David A.

1996-01-01

A thermal model, developed to predict seasonal nitrogen cycles on Triton, has been modified and applied to Pluto. The model was used to calculate the partitioning of nitrogen between surface frost deposits and the atmosphere, as a function of time for various sets of input parameters. Volatile transport was confirmed to have a significant effect on Pluto's climate as nitrogen moved around on a seasonal time scale between hemispheres, and sublimed into and condensed out of the atmosphere. Pluto's high obliquity was found to have a significant effect on the distribution of frost on its surface. Conditions that would lead to permanent polar caps on Triton were found to lead to permanent zonal frost bands on Pluto. In some instances, frost sublimed from the middle of a seasonal cap outward, resulting in a "polar bald spot". Frost which was darker than the substrate did not satisfy observables on Pluto, in contrast to our findings for Triton. Bright frost (brighter than the substrate) came closer to matching observables. Atmospheric pressure varied seasonally. The amplitudes, and to a lesser extent the phase, of the variation depended significantly on frost and substrate properties. Atmospheric pressure was found to be determined both by Pluto's distance from the sun and by the subsolar latitude. In most cases two peaks in atmospheric pressure were observed annually: a greater one associated with the sublimation of the north polar cap just as Pluto receded from perihelion, and a lesser one associated with the sublimation of the south polar cap as Pluto approached perihelion. Our model predicted frost-free dark substrate surface temperatures in the 50 to 60 K range, while frost temperatures typically ranged between 30 to 40 K. Temporal changes in frost coverage illustrated by our results, and changes in the viewing geometry of Pluto from the Earth, may be important for interpretation of ground-based measurements of Pluto's thermal emission.

Pluto in Hi-Def

NASA Image and Video Library

2008-01-24

This image demonstrates the first detection of Pluto using the high-resolution mode on the NASA New Horizons Long-Range Reconnaissance Imager. The mode provides a clear separation between Pluto and numerous nearby background stars.

Map of Pluto Surface

NASA Image and Video Library

1998-03-28

This image-based surface map of Pluto was assembled by computer image processing software from four separate images of Pluto disk taken with the European Space Agency Faint Object Camera aboard NASA Hubble Space Telescope.

Pluto's Atmospheric Figure from the P131.1 Stellar Occultation

NASA Astrophysics Data System (ADS)

Person, M. J.; Elliot, J. L.; Clancy, K. B.; Kern, S. D.; Salyk, C. V.; Tholen, D. J.; Pasachoff, J. M.; Babcock, B. A.; Souza, S. P.; Ticehurst, D. R.; Hall, D.; Roberts, L. C., Jr.; Bosh, A. S.; Buie, M. W.; Dunham, E. W.; Olkin, C. B.; Taylor, B.; Levine, S. E.; Eikenberry, S. S.; Moon, D.-S.; Osip, D. J.

2003-05-01

The stellar occultation by Pluto of the 15th magnitude star designated P131.1 (McDonald and Elliot, AJ, 119, 1999) on 2002 August 21 (UT) provided the first significant chance to compare Pluto's atmospheric structure to that determined from the 1988 occultation of P8 (Millis, et al., Icarus, 105, 282). The P131.1 occultation was observed from several stations in Hawaii and the western United States (Elliot et al., Nature, in press, 2003). Numerous occultation chords were obtained enabling us to examine Pluto's atmospheric figure. The light curves from the observations were analyzed together in the occultation coordinate system of Elliot et al., (AJ, 106, 2544). The Mauna Kea and Lick datasets straddle the center of Pluto's figure, providing strong constraints on model fits to cross sections of the atmospheric shape. In 1988, Millis (et al., Icarus, 105, 282) did not report any deviation from sphericity in Pluto's atmospheric figure. From the 2002 data, Pluto;s isobars at the radii probed by the occultation ( 1250 km) appear to be distorted from a circular cross-section. Least-squares fits to this cross-section by elliptical models reveal ellipticities in the range 0.05-0.08 although the shape may be more complex than ellipsoidal. The orientation of the distortion appears uncorrelated with Pluto;s rotational axis. Taken at face value, this ellipticity could imply wind speeds of up to twice the sonic speed ( 200 m/s), which would be difficult to explain. Similar distortions have been reported for Triton's atmosphere (Elliot, J. L., et al., Icarus 148, 347). This work has been supported in part by Research Corporation, the Air Force Research Laboratory, NSF, and NASA.

Volatile Transport on Pluto: First Results from the 2013 Observing Season

NASA Astrophysics Data System (ADS)

Buratti, B. J.; Dalba, P. A.; Hicks, M.; Chu, D.; O'Neill, A.; Chesley, J. P.

2013-12-01

With the New Horizons spacecraft due to encounter Pluto in slightly less than two years, close scrutiny of this dwarf ice planet has begun in earnest. Ground-based observations are especially critical for context and for a larger temporal excursion. Seasonal transport of volatiles should occur on Pluto, and this transport should be detectable through changes in its rotational light curve, once all variations due to viewing geometry have been modeled. Giving the steady increase observed in Pluto's atmospheric pressure over the past two decades, associated sublimation of frost from the surface has likely occurred, as predicted by volatile transport models. Rotational light curves of Pluto through time have been created for static frost models based on images from the Hubble Space Telescope. These models, which account for changes in viewing geometry, have been compared with observed light curves obtained between 1950 and 2013. No evidence for transport was evident prior to 2000. Observations from 2002 (Buie et al., 2010, Astron. J. 139, 1128) and 2007-2008 (Hicks et al. 2008, B.A.A.S. 40, 460) suggest changes in the frost pattern on Pluto's surface. New observations of Pluto's light curve from the 2013 season from Table Mountain Observatory show no evidence for the large transport of volatiles on Pluto's surface. Our data are the first measurement of a large opposition surge on Pluto similar to that seen on other icy bodies. Both Buie et al. (2010) and our observations from the 2012-2013 seasons show that Pluto is becoming more red in color. This observation makes sense if nitrogen is being removed from the surface to uncover a red, photolyzed substrate of methane. Funded by NASA.

Pluto and Charon: Surface Colors and Compositions - A Hypothesis

NASA Technical Reports Server (NTRS)

Cruikshank, D. P.

2016-01-01

The surface of Pluto displays an array of colors ranging from yellow to red to brown, while the surface of Charon is largely gray with a north polar zone of red color similar to regions on Pluto. Pluto's surface shows layers of intensely colored material in tilted and transported blocks, and fractured geo-graphical units. This arrangement suggests episodes of formation or deposition of that material interspersed with episodes of emplacement of ices having little or no color. The ices identified on the surfaces of these two bodies (N2, CH4, CO, C2H6, H2O on Pluto, and H2O and NH3 on Charon) are colorless, as are nearly all ices in a powdery state. The colors on Pluto probably arise from the in situ formation of a macro-molecular carbonaceous material generated by energetic processing of the ices on the surface. Laboratory experiments producing refractory tholins particularly relevant to Pluto explored the chemistry of both UV and low-energy electron bombardment of a mix of Pluto ices (N2:CH4:CO = 100:1:1). We can term this Pluto ice tholin PIT. Water ice in the crystalline state characterizes Charon's surface, and while most of Charon's surface is neutral in color, with geometric albedo approximately 0.38, the polar zone and a light cover of fainter but similar reddish color over some surface regions suggest a common origin with the colored material on Pluto. NH3 or NH3 x nH2O was identified from disk-integrated Earth-based spectra, and a few concentrated NH3 exposures have been found in the New Horizons spectral images.

Determination of the Charon/Pluto Mass Ratio from Center-of-Light Astrometry

NASA Technical Reports Server (NTRS)

Foust, Jeffrey A.; Elliot, J. L.; Olkin, Catherine B.; McDonald, Stephen W.; Dunham, Edward W.; Stone, Remington P. S.; McDonald, John S.; Stone, Ronald C.

1997-01-01

The Charon/Pluto mass ratio is a fundamental but poorly known parameter of the two-body system. Previous values for the mass ratio have ranged from 0.0837 plus or minus 0.0147 (Null et al., 1993, Astron. J. 105, 2319-2335) to 0.1566 plus or minus 0.0035 (Young et al., 1994, Icarus 108,186-199). We report here a new determination of the Charon/Pluto mass ratio, using five sets of groundbased images taken at four sites in support of Pluto occultation predictions. Unlike the Null et al. and Young et A determinations, where the centers of light for Pluto and Charon could be determined separately, this technique examines the motion of the center of light of the blended Pluto-Charon image. We compute the offsets of the observed center-of-light position of Pluto-Charon from the ephemeris position of the system and fit these offsets to a model of the Pluto-Charon system. The least-squares fits to the five data sets agree within their errors, and the weighted mean mass ratio is 0.117 plus or minus 0.006. The effects of errors in the Charon light fraction, semimajor axis, and ephemeris have been examined and are equal to only a small fraction of the formal error from the fit. This result is intermediate between those of Null et al., and Young et al. and matches a new value of 0.124 plus or minus 0.008 by Null and Owen (1996, Astron. J. 111, 1368-1381). The mass ratio and resulting individual masses and densities of Pluto and Charon are consistent with a collisional origin for the Pluto-Charon system.

The Icy Cold Heart of Pluto

NASA Astrophysics Data System (ADS)

Hamilton, Douglas P.

2015-11-01

The locations of large deposits of frozen volatiles on planetary surfaces are largely coincident with areas receiving the minimum annual influx of solar energy; familiar examples include the polar caps of Earth and Mars. For planets tilted by more than 45 degrees, however, the poles actually receive more energy than some other latitudes. Pluto, with its current obliquity of 119 degrees, has minima in its average annual insolation at +/- 27 degrees latitude, with ~1.5% more energy flux going to the equator and ~15% more to the poles. Remarkably, the fraction of annual solar energy incident on different latitudes depends only on the obliquity of the planet and not on any of its orbital parameters.Over millions of years, Pluto's obliquity varies sinusoidally from 102-126 degrees, significantly affecting the latitudinal profile of solar energy deposition. Roughly 1Myr ago, the poles received 15% more energy that today while the equator received 13% less. The energy flux to latitudes between 25-35 degrees is far more stable, remaining low over the presumably billions of years since Pluto acquired its current spin properties. Like the poles at Earth, these mid latitudes on Pluto should be favored for the long-term deposition of volatile ices. This is, indeed, the location of the bright icy heart of Pluto, Sputnik Planum.Reflected light and emitted thermal radiation from Charon increases annual insolation to one side of Pluto by of order 0.02%. Although small, the bulk of the energy is delivered at night to Pluto's cold equatorial regions. Furthermore, Charon's thermal infrared radiation is easily absorbed by icy deposits on Pluto, slowing deposition and facilitating sublimation of volatiles. We argue that the slight but persistent preference for ices to form and survive in the anti-Charon Pluto's heart.

Constraints on Pluto's Hazes from 2-Color Occultation Lightcurves

NASA Astrophysics Data System (ADS)

Hartig, Kara; Barry, T.; Carriazo, C. Y.; Cole, A.; Gault, D.; Giles, B.; Giles, D.; Hill, K. M.; Howell, R. R.; Hudson, G.; Loader, B.; Mackie, J. A.; Olkin, C. B.; Rannou, P.; Regester, J.; Resnick, A.; Rodgers, T.; Sicardy, B.; Skrutskie, M. F.; Verbiscer, A. J.; Wasserman, L. H.; Watson, C. R.; Young, E. F.; Young, L. A.; Buie, M. W.; Nelson, M.

2015-11-01

The controversial question of aerosols in Pluto's atmosphere first arose in 1988, when features in a Pluto occultation lightcurve were alternately attributed to haze opacity (Elliot et al. 1989) or a thermal inversion (Eshleman 1989). A stellar occultation by Pluto in 2002 was observed from several telescopes on Mauna Kea in wavelengths ranging from R- to K-bands (Elliot et al. 2003). This event provided compelling evidence for haze on Pluto, since the mid-event baseline levels were systematically higher at longer wavelengths (as expected if there were an opacity source that scattered more effectively at shorter wavelengths). However, subsequent occultations in 2007 and 2011 showed no significant differences between visible and IR lightcurves (Young et al. 2011).The question of haze on Pluto was definitively answered by direct imaging of forward-scattering aerosols by the New Horizons spacecraft on 14-JUL-2015. We report on results of a bright stellar occultation which we observed on 29-JUN-2015 in B- and H-bands from both grazing and central sites. As in 2007 and 2011, we see no evidence for wavelength-dependent extinction. We will present an analysis of haze parameters (particle sizes, number density profiles, and fractal aggregations), constraining models of haze distribution to those consistent with and to those ruled out by the occultation lightcurves and the New Horizons imaging.References:Elliot, J.L., et al., "Pluto's Atmosphere." Icarus 77, 148-170 (1989)Eshleman, V.R., "Pluto's Atmosphere: Models based on refraction, inversion, and vapor pressure equilibrium." Icarus 80 439-443 (1989)Elliot, J.L., et al., "The recent expansion of Pluto's atmosphere." Nature 424 165-168 (2003)Young, E.F., et al., "Search for Pluto's aerosols: simultaneous IR and visible stellar occultation observations." EPSC-DPS Joint Meeting 2011, held 2-7 October 2011 in Nantes, France (2011)

Destination pluto: New horizons performance during the approach phase

NASA Astrophysics Data System (ADS)

Flanigan, Sarah H.; Rogers, Gabe D.; Guo, Yanping; Kirk, Madeline N.; Weaver, Harold A.; Owen, William M.; Jackman, Coralie D.; Bauman, Jeremy; Pelletier, Frederic; Nelson, Derek; Stanbridge, Dale; Dumont, Phillip J.; Williams, Bobby; Stern, S. Alan; Olkin, Cathy B.; Young, Leslie A.; Ennico, Kimberly

2016-11-01

The New Horizons spacecraft began its journey to the Pluto-Charon system on January 19, 2006 on-board an Atlas V rocket from Cape Canaveral, Florida. As the first mission in NASA's New Frontiers program, the objective of the New Horizons mission is to perform the first exploration of ice dwarfs in the Kuiper Belt, extending knowledge of the solar system to include the icy "third zone" for the first time. Arriving at the correct time and correct position relative to Pluto on July 14, 2015 depended on the successful execution of a carefully choreographed sequence of events. The Core command sequence, which was developed and optimized over multiple years and included the highest-priority science observations during the closest approach period, was contingent on precise navigation to the Pluto-Charon system and nominal performance of the guidance and control (G&C) subsystem. The flyby and gravity assist of Jupiter on February 28, 2007 was critical in placing New Horizons on the path to Pluto. Once past Jupiter, trajectory correction maneuvers (TCMs) became the sole source of trajectory control since the spacecraft did not encounter any other planetary bodies along its flight path prior to Pluto. During the Pluto approach phase, which formally began on January 15, 2015, optical navigation images were captured primarily with the Long Range Reconnaissance Imager to refine spacecraft and Pluto-Charon system trajectory knowledge, which in turn was used to design TCMs. Orbit determination solutions were also used to update the spacecraft's on-board trajectory knowledge throughout the approach phase. Nominal performance of the G&C subsystem, accurate TCM designs, and high-quality orbit determination solutions resulted in final Pluto-relative B-plane arrival conditions that facilitated a successful first reconnaissance of the Pluto-Charon system.

Hubble Finds Two Chaotically Tumbling Pluto Moons

NASA Image and Video Library

2015-06-03

This computer animation illustrates how Pluto's moon Nix changes its spin unpredictably as it orbits the "double planet" Pluto-Charon. The view is from the surface of Pluto as the moon circles the Pluto-Charon system. This is a time-lapse view of the moon, compressing four years of motion into two minutes, with one complete orbit of Pluto-Charon every two seconds. (The apparent star movement rate is greatly slowed down for illustration purposes.) The animation is based on dynamical models of spinning bodies in complex gravitational fields — like the field produced by Pluto and Charon's motion about each other. Astronomers used this simulation to try to understand the unpredictable changes in reflected light from Nix as it orbits Pluto-Charon. They also found that Pluto's moon Hydra also undergoes chaotic spin. The football shape of both moons contributes to their wild motion. The consequences are that if you lived on either moon, you could not predict the time or direction the sun would rise the next morning. (The moon is too small for Hubble to resolve surface features, and so the surface textures used here are purely for illustration purposes.) Credit: NASA, ESA, M. Showalter (SETI Institute), and G. Bacon (STScI) Read more: www.nasa.gov/press-release/nasa-s-hubble-finds-pluto-s-mo... NASA image use policy. NASA Goddard Space Flight Center enables NASA’s mission through four scientific endeavors: Earth Science, Heliophysics, Solar System Exploration, and Astrophysics. Goddard plays a leading role in NASA’s accomplishments by contributing compelling scientific knowledge to advance the Agency’s mission. Follow us on Twitter Like us on Facebook Find us on Instagram

The Orbits and Masses of Pluto's Satellites

NASA Astrophysics Data System (ADS)

Jacobson, Robert A.; Brozovic, M.

2012-10-01

We have fit numerically integrated orbits of Pluto's satellites, Charon, Nix, Hydra, and S/2011 (134340) 1, to an extensive set of astrometric, mutual event, and stellar occultation observations over the time interval April 1965 to July 2011. We did not include the newly discovered satellite S/2012 (134340) 1 because its observation set is insufficient to constrain a numerically integrated orbit. The data set contains all of the HST observations of Charon relative to Pluto which have been corrected for the Pluto center-of-figure center-of-light (COF) offset due to the Pluto albedo variations (Buie et al. 2012 AJ submitted). Buie et al. (2010 AJ 139, 1117 and 1128) discuss the development of the albedo model and the COF offset. We applied COF offset corrections to the remainder of the Pluto relative observations where applicable. The dual stellar occultations in 2008 and 2011 provided precise Pluto_Charon relative positions. We obtain a well determined value for the Pluto system mass, however, the lack of orbital resonances in the system makes it difficult to determine the satellite masses. The primary source of information for the Charon mass is a small quantity of absolute position measurements which are sensitive to the independent motions of Pluto and Charon about the system barycenter. The long term dynamical interaction among the satellites yields a weak determination of Hydra's mass; the masses of the other two satellites are found to be small but indeterminate. We have delivered ephemerides based on our integrated orbits to the New Horizons project along with their expected uncertainties at the time of the New Horizons encounter with the Pluto system. Acknowledgments: The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

The Pluto system: Initial results from its exploration by New Horizons.

PubMed

Stern, S A; Bagenal, F; Ennico, K; Gladstone, G R; Grundy, W M; McKinnon, W B; Moore, J M; Olkin, C B; Spencer, J R; Weaver, H A; Young, L A; Andert, T; Andrews, J; Banks, M; Bauer, B; Bauman, J; Barnouin, O S; Bedini, P; Beisser, K; Beyer, R A; Bhaskaran, S; Binzel, R P; Birath, E; Bird, M; Bogan, D J; Bowman, A; Bray, V J; Brozovic, M; Bryan, C; Buckley, M R; Buie, M W; Buratti, B J; Bushman, S S; Calloway, A; Carcich, B; Cheng, A F; Conard, S; Conrad, C A; Cook, J C; Cruikshank, D P; Custodio, O S; Dalle Ore, C M; Deboy, C; Dischner, Z J B; Dumont, P; Earle, A M; Elliott, H A; Ercol, J; Ernst, C M; Finley, T; Flanigan, S H; Fountain, G; Freeze, M J; Greathouse, T; Green, J L; Guo, Y; Hahn, M; Hamilton, D P; Hamilton, S A; Hanley, J; Harch, A; Hart, H M; Hersman, C B; Hill, A; Hill, M E; Hinson, D P; Holdridge, M E; Horanyi, M; Howard, A D; Howett, C J A; Jackman, C; Jacobson, R A; Jennings, D E; Kammer, J A; Kang, H K; Kaufmann, D E; Kollmann, P; Krimigis, S M; Kusnierkiewicz, D; Lauer, T R; Lee, J E; Lindstrom, K L; Linscott, I R; Lisse, C M; Lunsford, A W; Mallder, V A; Martin, N; McComas, D J; McNutt, R L; Mehoke, D; Mehoke, T; Melin, E D; Mutchler, M; Nelson, D; Nimmo, F; Nunez, J I; Ocampo, A; Owen, W M; Paetzold, M; Page, B; Parker, A H; Parker, J W; Pelletier, F; Peterson, J; Pinkine, N; Piquette, M; Porter, S B; Protopapa, S; Redfern, J; Reitsema, H J; Reuter, D C; Roberts, J H; Robbins, S J; Rogers, G; Rose, D; Runyon, K; Retherford, K D; Ryschkewitsch, M G; Schenk, P; Schindhelm, E; Sepan, B; Showalter, M R; Singer, K N; Soluri, M; Stanbridge, D; Steffl, A J; Strobel, D F; Stryk, T; Summers, M E; Szalay, J R; Tapley, M; Taylor, A; Taylor, H; Throop, H B; Tsang, C C C; Tyler, G L; Umurhan, O M; Verbiscer, A J; Versteeg, M H; Vincent, M; Webbert, R; Weidner, S; Weigle, G E; White, O L; Whittenburg, K; Williams, B G; Williams, K; Williams, S; Woods, W W; Zangari, A M; Zirnstein, E

2015-10-16

The Pluto system was recently explored by NASA's New Horizons spacecraft, making closest approach on 14 July 2015. Pluto's surface displays diverse landforms, terrain ages, albedos, colors, and composition gradients. Evidence is found for a water-ice crust, geologically young surface units, surface ice convection, wind streaks, volatile transport, and glacial flow. Pluto's atmosphere is highly extended, with trace hydrocarbons, a global haze layer, and a surface pressure near 10 microbars. Pluto's diverse surface geology and long-term activity raise fundamental questions about how small planets remain active many billions of years after formation. Pluto's large moon Charon displays tectonics and evidence for a heterogeneous crustal composition; its north pole displays puzzling dark terrain. Small satellites Hydra and Nix have higher albedos than expected. Copyright © 2015, American Association for the Advancement of Science.

Observational Limits for Rings and Debris at Pluto from New Horizons

NASA Astrophysics Data System (ADS)

Throop, Henry B.; Lauer, Tod R.; Showalter, Mark R.; Weaver, Harold A.; Stern, S. Alan; Spencer, John R.; Buie, Marc W.; Hamilton, Douglas P.; Porter, Simon Bernard; Verbiscer, Anne J.; Young, Leslie; Olkin, Catherine; Ennico, Kimberly; New Horizons Science Team

2017-10-01

NASA's New Horizons missions flew past Pluto on July 14, 2015. New Horizons conducted an extensive search for orbital material at Pluto, using deep imaging at backscatter and forward-scatter, direct in situ dust detector measurements, and stellar occultations. We searched the entire region from the surface of Pluto outward to the Pluto-Charon Hill radius (6.4 x 106 km = 100 times Hydra's orbital radius), using the spacecraft's LORRI and MVIC cameras.No material was found to a normal I/F limit of 2 x 10-8 for 1500 km-wide rings, and 7 x 10-9 for 12,000 km-wide rings. Our results are consistent with dynamical studies that show the lifetime of dust in the Pluto system is short, with the loss dominated by solar radiation pressure and gravitational perturbations.

Reorientation and faulting of Pluto due to volatile loading within Sputnik Planitia.

PubMed

Keane, James T; Matsuyama, Isamu; Kamata, Shunichi; Steckloff, Jordan K

2016-12-01

Pluto is an astoundingly diverse, geologically dynamic world. The dominant feature is Sputnik Planitia-a tear-drop-shaped topographic depression approximately 1,000 kilometres in diameter possibly representing an ancient impact basin. The interior of Sputnik Planitia is characterized by a smooth, craterless plain three to four kilometres beneath the surrounding rugged uplands, and represents the surface of a massive unit of actively convecting volatile ices (N 2 , CH 4 and CO) several kilometres thick. This large feature is very near the Pluto-Charon tidal axis. Here we report that the location of Sputnik Planitia is the natural consequence of the sequestration of volatile ices within the basin and the resulting reorientation (true polar wander) of Pluto. Loading of volatile ices within a basin the size of Sputnik Planitia can substantially alter Pluto's inertia tensor, resulting in a reorientation of the dwarf planet of around 60 degrees with respect to the rotational and tidal axes. The combination of this reorientation, loading and global expansion due to the freezing of a possible subsurface ocean generates stresses within the planet's lithosphere, resulting in a global network of extensional faults that closely replicate the observed fault networks on Pluto. Sputnik Planitia probably formed northwest of its present location, and was loaded with volatiles over million-year timescales as a result of volatile transport cycles on Pluto. Pluto's past, present and future orientation is controlled by feedbacks between volatile sublimation and condensation, changing insolation conditions and Pluto's interior structure.

Radio Occultation Measurements of Pluto's Atmosphere with New Horizons

NASA Astrophysics Data System (ADS)

Hinson, D. P.; Linscott, I.; Tyler, G. L.; Bird, M. K.; Paetzold, M.; Strobel, D. F.; Summers, M. E.; Woods, W. W.; Stern, A.; Weaver, H. A., Jr.; Olkin, C.; Young, L. A.; Ennico Smith, K.; Gladstone, R.; Greathouse, T.; Kammer, J.; Parker, A. H.; Parker, J. W.; Retherford, K. D.; Schindhelm, E.; Singer, K. N.; Steffl, A.; Tsang, C.; Versteeg, M.

2015-12-01

The reconnaissance of the Pluto System by New Horizons included radio occultations at both Pluto and Charon. This talk will present the latest results from the Pluto occultation. The REX instrument onboard New Horizons received and recorded uplink signals from two 70-m antennas and two 34-m antennas of the NASA Deep Space Network - each transmitting 20 kW at 4.2-cm wavelength - during a diametric occultation by Pluto. At the time this was written only a short segment of data at occultation entry (193°E, 17°S) was available for analysis. The REX measurements extend unequivocally to the surface, providing the first direct measure of the surface pressure and the temperature structure in Pluto's lower atmosphere. Preliminary analysis yields a surface pressure of about 10 microbars, smaller than expected. Data from occultation exit (16°E, 15°N) are scheduled to arrive on the ground in late August 2015. Those observations will yield an improved estimate of the surface pressure, a second temperature profile, and a measure of the diameter of Pluto with a precision of a few hundred meters.

Discovery of two new satellites of Pluto.

PubMed

Weaver, H A; Stern, S A; Mutchler, M J; Steffl, A J; Buie, M W; Merline, W J; Spencer, J R; Young, E F; Young, L A

2006-02-23

Pluto's first known satellite, Charon, was discovered in 1978. It has a diameter (approximately 1,200 km) about half that of Pluto, which makes it larger, relative to its primary, than any other moon in the Solar System. Previous searches for other satellites around Pluto have been unsuccessful, but they were not sensitive to objects less, similar150 km in diameter and there are no fundamental reasons why Pluto should not have more satellites. Here we report the discovery of two additional moons around Pluto, provisionally designated S/2005 P 1 (hereafter P1) and S/2005 P 2 (hereafter P2), which makes Pluto the first Kuiper belt object known to have multiple satellites. These new satellites are much smaller than Charon, with estimates of P1's diameter ranging from 60 km to 165 km, depending on the surface reflectivity; P2 is about 20 per cent smaller than P1. Although definitive orbits cannot be derived, both new satellites appear to be moving in circular orbits in the same orbital plane as Charon, with orbital periods of approximately 38 days (P1) and approximately 25 days (P2).

Changes in Pluto's Atmosphere Revealed by Occultations

NASA Astrophysics Data System (ADS)

Sicardy, Bruno; Widemann, Thomas; Lellouch, Emmanuel; Veillet, Christian; Colas, Francois; Roques, Francoise; Beisker, Wolfgang; Kretlow, Mike; Cuillandre, Jean-Charles; Hainaut, Olivier

After the discovery and study of Pluto's tenuous atmosphere in 1985 and 1988 with stellar occultations 14 years were necessary before two other occultations by the planet could be observed on 20 July 2002 and 21 August 2002 from Northern Chile with a portable telescope and from CFHT in Hawaii respectively. These occultations reveal drastric changes in Pluto's nitrogen atmosphere whose pressure increased by a factor two or more since 1988. In spite of an increasing distance to the Sun (and a correlated decrease of solar energy input at Pluto) this increase can be explained by the fact that Pluto's south pole went from permanent darkness to permanent illumination between 1988 and 2002. This might cause the sublimation of the south polar cap and the increase of pressure which could go on till 2015 according to current nitrogen cycle models. Furthermore we detect temperature contrasts between the polar and the equatorial regions probed on Pluto possibly caused by different diurnally averaged insolations at those locations. Finally spikes observed in the light curves reveal a dynamical activity in Pluto's atmosphere.

Occultation Lightcurves for Selected Pluto Volatile Transport Models

NASA Astrophysics Data System (ADS)

Young, L. A.

2004-11-01

The stellar occultations by Pluto in 1988 and 2002 are demonstrably sensitive to changes in Pluto's atmosphere near one microbar (Elliot and Young 1992, AJ 103, 991; Elliot et al. 2003, Nature 424, 165; Sicardy 2003, Nature 424, 168). However, Pluto volatile-transport models focus on the changes in the atmospheric pressure at the surface (e.g., Hansen and Paige 1996, Icarus 20, 247; Stansberry and Yelle 1999, Icarus 141, 299). What's lacking is a connection between predictions about the surface properties and either temperature and pressure profiles measurable from stellar occultations, or the occultation light curve morphology itself. Radiative-conductive models can illuminate this connection. I will illustrate how Pluto's changing surface pressure, temperature, and heliocentric distance may affect occultation light curves for a selection of existing volatile transport models. Changes in the light curve include the presence or absence of an observable ``kink'' (or departure from an isothermal light curve), the appearance of non-zero minimum flux levels, and the detectability of the solid surface. These light curves can serve as examples of what we may anticipate during the upcoming Pluto occultation season, as Pluto crosses the galactic plane.

Pluto Big Heart in Color

NASA Image and Video Library

2015-07-14

Pluto nearly fills the frame in this image from NASA New Horizons spacecraft, taken on July 13, 2015. This is the last and most detailed image sent to Earth before the spacecraft closest approach to Pluto on July 14.

Pluto Bladed Terrain in 3-D

NASA Image and Video Library

2016-03-31

One of the strangest landforms spotted by NASA New Horizons spacecraft when it flew past Pluto last July was the bladed terrain just east of Tombaugh Regio, the informal name given to Pluto large heart-shaped surface feature.

Image Analysis of the 2012 Pluto (Near) Occultation

DTIC Science & Technology

2013-09-01

Image Analysis of the 2012 Pluto (Near) Occultation Keith T. Knox Air Force Research Laboratory ABSTRACT Imagery was gathered at the AMOS...observatory on the 3.6-meter telescope for the expected occultation of a star by the dwarf planet, Pluto , on 29 June 2012. The imagery was taken at...5 Hz for 40 minutes before and after the expected time of occultation. The initial analysis of the photometry indicated that Pluto did not occult

Astrometrical observations of Pluto-Charon system with the automated telescopes of Pulkovo observatory

NASA Astrophysics Data System (ADS)

Slesarenko, V. Yu.; Bashakova, E. A.; Devyatkin, A. V.

2016-03-01

The space probe "New Horizons" was launched on 19th of January 2006 in order to study Pluto and its moons. Spacecraft performed close fly-by to Pluto on 14th of July 2015 and obtained the most detailed images of Pluto and its moon until this moment. At the same time, observation obtained by the ground-based telescopes may also be helpful for the research of such distant system. Thereby, the Laboratory of observational astrometry of Pulkovo Observatory of RAS made a decision to reprocess observations obtained during last decade. More than 350 positional observations of Pluto-Charon system were carried out with the mirror astrograph ZA-320M at Pulkovo and Maksutov telescope MTM-500M near Kislovodsk. These observations were processed by means of software system APEX-II developed in Pulkovo observatory and numerical simulations were performed to calculate the differences between positions of photocenter and barycenter of Pluto-Charon system.

17. Photocopy of photograph. VIEW OF WORKERS IN EAST OPERATING ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

17. Photocopy of photograph. VIEW OF WORKERS IN EAST OPERATING GALLERY USING MANIPULATOR ARMS AT STATION E-108. Photographer unknown, ca. 1965, original photograph and negative on file at the Remote Sensing Laboratory, Department of Energy, Nevada Operations Office. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

ScienceCast 26: Visit to Pluto

NASA Image and Video Library

2011-09-02

Pluto is a world of mystery waiting to be visited for the 1st time. NASA's New Horizons probe is racing across the solar system for a close encounter that could alter what researchers "know" about Pluto and other small worlds.

Pluto is the new Mars!

NASA Technical Reports Server (NTRS)

Moore, Jeffrey M.; Mckinnon, William B.; Spencer, John R.; Howard, Alan D.; Grundy, William M.; Stern, S. Alan; Weaver, Harold A.; Young, Leslie A.; Ennico, Kimberly; Olkin, Cathy

2016-01-01

Data from NASA's New Horizons encounter with Pluto in July 2015 revealed an astoundingly complex world. The surface seen on the encounter hemisphere ranged in age from ancient to recent. A vast craterless plain of slowly convecting solid nitrogen resides in a deep primordial impact basin, reminiscent of young enigmatic deposits in Mars' Hellas basin. Like Mars, regions of Pluto are dominated by valleys, though the Pluto valleys are thought to be carved by nitrogen glaciers. Pluto has fretted terrain and halo craters. Pluto is cut by tectonics of several different ages. Like Mars, vast tracts on Pluto are mantled by dust and volatiles. Just as on Mars, Pluto has landscapes that systematically vary with latitude due to past and present seasonal (and mega-seasonal) effects on two major volatiles. On Mars, those volatiles are H2O and CO2; on Pluto they are CH4 and N2. Like Mars, some landscapes on Pluto defy easy explanation. In the Plutonian arctic there is a region of large (approx. 40 km across) deep (approx. 3-4 km) pits that probably could not be formed by sublimation, or any other single process, alone. Equally bizarre is the Bladed terrain, which is composed of fields of often roughly aligned blade-like ridges covering the flanks and crests of broad regional swells. Topping the unexpected are two large mounds approximately150 km across, approx. 5-6 km high, with great central depressions at their summits. The central depressions are almost as deep as the mounds are tall. These mounds have many of the characteristics of volcanic mountains seen on Mars and elsewhere in the inner solar system. Hypotheses for the formation of these Plutonian mounds so far all have challenges, principally revolving around the need for H2O ice to support their relief and the difficulty imagining mechanisms that would mobilize H2O. From the perspective of one year after the encounter, our appreciation of the extent of Pluto's diversity and complexity is quite reminiscent of the perspective the science community had of Mars, with similar quality data sets, soon after the early reconnaissance of that planet in the late 1960s and early 70s. So certainly in this sense, Pluto is the new Mars.

Pluto in Twilight

NASA Image and Video Library

2015-09-10

This image of Pluto from NASA's New Horizons spacecraft, processed in two different ways, shows how Pluto's bright, high-altitude atmospheric haze produces a twilight that softly illuminates the surface before sunrise and after sunset, allowing the sensitive cameras on New Horizons to see details in nighttime regions that would otherwise be invisible. The right-hand version of the image has been greatly brightened to bring out faint details of rugged haze-lit topography beyond Pluto's terminator, which is the line separating day and night. The image was taken as New Horizons flew past Pluto on July 14, 2015, from a distance of 50,000 miles (80,000 kilometers). http://photojournal.jpl.nasa.gov/catalog/PIA19931

NASA Researchers Discover “Bladed Terrain” on Pluto is Made of Frozen Methane (Video News File)

NASA Image and Video Library

2017-09-22

NASA has identified large formations of frozen methane on the surface of Pluto that are as tall as skyscrapers. Researchers at NASA’s Ames Research Center in Silicon Valley used high resolution maps from the New Horizons flyby of Pluto in 2015 to understand these dramatic structures. The “bladed terrain” occurs only at high altitudes and in the region around the equator of Pluto. These jagged spires are thought to be created by an erosion process as the methane ice sublimates into gas. Researchers hope to use their findings to fill in the details of the areas of Pluto that were only measured in low resolution.

Pluto behaving badly: false beliefs and their consequences.

PubMed

Berkowitz, Shari R; Laney, Cara; Morris, Erin K; Garry, Maryanne; Loftus, Elizabeth F

2008-01-01

We exposed college students to suggestive materials in order to lead them to believe that, as children, they had a negative experience at Disneyland involving the Pluto character. A sizable minority of subjects developed a false belief or memory that Pluto had uncomfortably licked their ear. Suggestions about a positive experience with Pluto led to even greater acceptance of a lovable ear-licking episode. False beliefs and memories had repercussions; those seduced by the bad suggestions were not willing to pay as much for a Pluto souvenir. These findings are among the first to demonstrate that false beliefs can have repercussions for people, meaning that they can influence their later thoughts, beliefs, and behaviors.

Volatile Transport in Pluto's Super Seasons

NASA Astrophysics Data System (ADS)

Earle, Alissa M.; Binzel, Richard; Young, Leslie; Stern, S. Alan; Olkin, Catherine B.; Ennico, Kimberly; Moore, Jeffrey M.; Weaver, Harold A.; NASA New Horizons Composition Team, The NASA New Horizons GGI Team

2016-10-01

The data returned from NASA's New Horizons' reconnaissance of the Pluto system shows striking albedo variations from polar to equatorial latitudes as well as sharp boundaries for longitudinal variations. Pluto has a high obliquity (currently around 119 degrees) which varies by more than 23 degrees (between roughly 103 and 127 degrees) over a period of less than 3 million years. These obliquity properties, combined with Pluto's orbital regression in longitude of perihelion (360 degrees over 3.7 million years), create epochs of "Super Seasons" on Pluto. A "Super Season" occurs, for example, when Pluto happens to be pole-on towards the Sun at the same time as perihelion. In such a case, one pole experiences a short, intense summer (relative to its long-term average) followed by a longer than average period of winter darkness. By complement, the other pole experiences a much longer, but less intense summer and short winter season. We explore the relationship between albedo variations and volatile transport for the current epoch as well as historical epochs during which Pluto experienced these "Super Seasons". Our investigation suggests Pluto's orbit creates the potential for runaway albedo variations, particularly in the equatorial region, which would create and support stark longitudinal contrasts like the ones we see between the informally named Tombaugh and Cthulhu Regios.This work was supported by the NASA New Horizons mission.

The State of Pluto's Bulk Atmosphere at the Time of the New Horizons Encounter

NASA Astrophysics Data System (ADS)

Resnick, Aaron C.; Barry, T.; Buie, M. W.; Carriazo, C. Y.; Cole, A.; Gault, D.; Giles, B.; Giles, D.; Hartig, K.; Hill, K.; Howell, R. R.; Hudson, G.; Loader, B.; Mackie, J.; Nelson, M.; Olkin, C.; Register, J.; Rodgers, T.; Sicardy, B.; Skrutskie, M.; Verbiscer, A.; Wasserman, L.; Watson, C.; Young, E.; Young, L.; Zalucha, A.

2015-11-01

On 29-JUL-2015, our team - plus many critical amateur astronomers - observed a stellar occultation by Pluto from sites in Australia and New Zealand. This event was remarkable for two reasons: it preceded the New Horizons flyby of Pluto by just two weeks, and the occulted star was about 10x brighter than Pluto itself, by far the brightest Pluto occultation event observed to date. The separation of ground sites spanned nearly 900 km with respect to the central chord, allowing a good geometric solution for the shadow path. The lightcurves show some inflection points and broad "fangs" that are characteristic of perturbations in the temperature profile. Preliminary fits show that the temperature profile derived from a 2006 occultation (Young et al. 2008) reproduces the 29-JUN-2015 lightcurves well. Assuming a surface radius of 1187 km for Pluto, we find that the surface pressure is 18 +/- 3 µbar. This pressure indicates that Pluto's surface has not yet started to cool down, despite a decrease in absorbed solar flux of more than 17% since perihelion in 1988. A surface pressure of 18 µbar would correspond to a nitrogen ice surface temperature of 38.0 K.References:Young, E.F., et al. "Vertical Structure in Pluto's Atmosphere from the 2006 June 12 Stellar Occultation," AJ 136 1757-1769 (2008)

Two Faces of Pluto

NASA Image and Video Library

2015-07-01

This pair of approximately true color images of Pluto and its big moon Charon, taken by NASA's New Horizons spacecraft, highlight the dramatically different appearance of different sides of the dwarf planet, and reveal never-before-seen details on Pluto's varied surface. The views were made by combining high-resolution black-and-white images from the Long Range Reconnaissance Imager (LORRI) with color information from the lower-resolution color camera that is part of the Ralph instrument. The left-hand image shows the side of Pluto that always faces away from Charon -- this is the side that will be seen at highest resolution by New Horizons when it makes its close approach to Pluto on July 14th. This hemisphere is dominated by a very dark region that extends along the equator and is redder than its surroundings, alongside a strikingly bright, paler-colored region which straddles the equator on the right-hand side of the disk. The opposite hemisphere, the side that faces Charon, is seen in the right-hand image. The most dramatic feature on this side of Pluto is a row of dark dots arranged along the equator. The origin of all these features is still mysterious, but may be revealed in the much more detailed images that will be obtained as the spacecraft continues its approach to Pluto. In both images, Charon shows a darker and grayer color than Pluto, and a conspicuous dark polar region. The left-hand image was obtained at 5:37 UT on June 25th 2015, at a distance from Pluto of 22.9 million kilometers (14.3 million miles) and has a central longitude of 152 degrees. The right-hand image was obtained at 23:15 UT on June 27th 2015, at a distance from Pluto of 19.7 million kilometers (12.2 million miles) with a central longitude of 358 degrees. Insets show the orientation of Pluto in each image -- the solid lines mark the equator and the prime meridian, which is defined to be the longitude that always faces Charon. The smallest visible features are about 200 km (120 miles) across. http://photojournal.jpl.nasa.gov/catalog/PIA19693

Final Hazard Search

NASA Image and Video Library

2015-07-08

This single frame from a four-frame movie shows New Horizons' final deep search for hazardous material around Pluto, obtained on July 1, 2015. These data allow a highly sensitive search for any new moons. The images were taken with the spacecraft's Long Range Reconnaissance Imager (LORRI) over a 100-minute period, and were the final observations in the series of dedicated searches for hazards in the Pluto system which began on May 11. The images show all five known satellites of Pluto moving in their orbits around the dwarf planet, but analysis of these data has so far not revealed the existence of any additional moons. This means that any undiscovered Plutonian moons further than a few thousand miles from Pluto must be smaller than about 1 mile (1.6 kilometers) in diameter, if their surfaces have similar brightness to Pluto's big moon Charon. For comparison, Pluto's faintest known moon, Styx, which is conspicuous in the lower left quadrant of these images, is about 4 miles (7 kilometers) across, assuming the same surface brightness. The absence of additional moons, and also the absence of detectable rings in the hazard search data, imply that the spacecraft is very unlikely to be damaged by collisions with rings, or dust particles ejected from moons, during its high-speed passage through the Pluto system. The four movie frames were taken at 16:28, 16:38, 17:52, and 18:04 UTC on July 1, from a range of 9.4 million miles (15.2 million kilometers). Each frame is a mosaic of four sets of overlapping images, with a total exposure time of 120 seconds. The images have been heavily processed to remove the glare of Pluto and Charon, and the dense background of stars, though blemishes remain at the locations of many of the brighter stars. The "tails" extending to the right or downward from Pluto and Charon are camera artifacts caused by the extreme overexposure of both objects. Pluto and its five moons Charon, Styx, Nix, Kerberos and Hydra are identified by their initials, and their orbits around the center of gravity of the system (which is located just outside Pluto itself) are also shown. http://photojournal.jpl.nasa.gov/catalog/PIA19701

Blue Rays: New Horizons High-Res Farewell to Pluto

NASA Image and Video Library

2017-03-24

This is the highest-resolution color departure shot of Pluto's receding crescent from NASA's New Horizons spacecraft, taken when the spacecraft was 120,000 miles (200,000 kilometers) away from Pluto. Shown in approximate true color, the picture was constructed from a mosaic of six black-and-white images from the Long Range Reconnaissance Imager (LORRI), with color added from a lower resolution Ralph/Multispectral Visible Imaging Camera (MVIC) color image, all acquired between 15:20 and 15:45 UT -- about 3.5 hours after closest approach to Pluto -- on July 14, 2015. The resolution of the LORRI images is about 0.6 miles (1 kilometer) per pixel; the sun illuminates the scene from the other side of Pluto and somewhat toward the top of this image. The image is dominated by spectacular layers of blue haze in Pluto's atmosphere. Scientists believe the haze is a photochemical smog resulting from the action of sunlight on methane and other molecules in Pluto's atmosphere, producing a complex mixture of hydrocarbons such as acetylene and ethylene. These hydrocarbons accumulate into small haze particles, a fraction of a micrometer in size, which preferentially scatter blue sunlight -- the same process that can make haze appear bluish on Earth. As they settle down through the atmosphere, the haze particles form numerous intricate, horizontal layers, some extending for hundreds of miles around large portions of the limb of Pluto. The haze layers extend to altitudes of over 120 miles (200 kilometers). Pluto's circumference is 4,667 miles (7,466 kilometers). Adding to the beauty of this picture are mountains and other topographic features on Pluto's surface that are silhouetted against the haze near the top of the image. Sunlight casts dramatic and beautiful finger-like shadows from many of these features onto the haze (especially on the left, near the 11 o'clock position), forming crepuscular rays like those often seen in Earth's atmosphere near sunrise or sunset. https://photojournal.jpl.nasa.gov/catalog/PIA21590

Pluto in 3-D

NASA Image and Video Library

2015-10-23

Global stereo mapping of Pluto surface is now possible, as images taken from multiple directions are downlinked from NASA New Horizons spacecraft. Stereo images will eventually provide an accurate topographic map of most of the hemisphere of Pluto seen by New Horizons during the July 14 flyby, which will be key to understanding Pluto's geological history. This example, which requires red/blue stereo glasses for viewing, shows a region 180 miles (300 kilometers) across, centered near longitude 130 E, latitude 20 N (the red square in the global context image). North is to the upper left. The image shows an ancient, heavily cratered region of Pluto, dotted with low hills and cut by deep fractures, which indicate extension of Pluto's crust. Analysis of these stereo images shows that the steep fracture in the upper left of the image is about 1 mile (1.6 kilometers) deep, and the craters in the lower right part of the image are up to 1.3 miles (2.1 km) deep. Smallest visible details are about 0.4 miles (0.6 kilometers) across. You will need 3D glasses to view this image showing an ancient, heavily cratered region of Pluto. http://photojournal.jpl.nasa.gov/catalog/PIA20032

Astrometry of Pluto from 1930-1951 observations: The Lampland plate collection

DOE Office of Scientific and Technical Information (OSTI.GOV)

Buie, Marc W.; Folkner, William M., E-mail: buie@boulder.swri.edu, E-mail: william.m.folkner@jpl.nasa.gov

We present a new analysis of 843 photographic plates of Pluto taken by Carl Lampland at Lowell Observatory from 1930–1951. This large collection of plates contains useful astrometric information that improves our knowledge of Pluto's orbit. This improvement provides critical support to the impending flyby of Pluto by New Horizons. New Horizons can do inbound navigation of the system to improve its targeting. This navigation is capable of nearly eliminating the sky-plane errors but can do little to constrain the time of closest approach. Thus the focus on this work was to better determine Pluto's heliocentric distance and to determinemore » the uncertainty on that distance with a particular eye to eliminating systematic errors that might have been previously unrecognized. This work adds 596 new astrometric measurements based on the USNO CCD Astrograph Catalog 4. With the addition of these data the uncertainty of the estimated heliocentric position of Pluto in Developmental Ephemerides 432 (DE432) is at the level of 1000 km. This new analysis gives us more confidence that these estimations are accurate and are sufficient to support a successful flyby of Pluto by New Horizons.« less

Astrometry of Pluto from 1930-1951 Observations: the Lampland Plate Collection

NASA Astrophysics Data System (ADS)

Buie, Marc W.; Folkner, William M.

2015-01-01

We present a new analysis of 843 photographic plates of Pluto taken by Carl Lampland at Lowell Observatory from 1930-1951. This large collection of plates contains useful astrometric information that improves our knowledge of Pluto's orbit. This improvement provides critical support to the impending flyby of Pluto by New Horizons. New Horizons can do inbound navigation of the system to improve its targeting. This navigation is capable of nearly eliminating the sky-plane errors but can do little to constrain the time of closest approach. Thus the focus on this work was to better determine Pluto's heliocentric distance and to determine the uncertainty on that distance with a particular eye to eliminating systematic errors that might have been previously unrecognized. This work adds 596 new astrometric measurements based on the USNO CCD Astrograph Catalog 4. With the addition of these data the uncertainty of the estimated heliocentric position of Pluto in Developmental Ephemerides 432 (DE432) is at the level of 1000 km. This new analysis gives us more confidence that these estimations are accurate and are sufficient to support a successful flyby of Pluto by New Horizons.

Pluto's Far Ultraviolet Spectrum and Airglow Emissions

NASA Astrophysics Data System (ADS)

Steffl, A.; Schindhelm, E.; Kammer, J.; Gladstone, R.; Greathouse, T. K.; Parker, J. W.; Strobel, D. F.; Summers, M. E.; Versteeg, M. H.; Ennico Smith, K.; Hinson, D. P.; Linscott, I.; Olkin, C.; Parker, A. H.; Retherford, K. D.; Singer, K. N.; Tsang, C.; Tyler, G. L.; Weaver, H. A., Jr.; Woods, W. W.; Young, L. A.; Stern, A.

2015-12-01

The Alice far ultraviolet spectrograph on the New Horizons spacecraft is the second in a family of six instruments in flight on, or under development for, NASA and ESA missions. Here, we present initial results from the Alice observations of Pluto during the historic flyby. Pluto's far ultraviolet spectrum is dominated by sunlight reflected from the surface with absorption by atmospehric constituents. We tentatively identify C2H2 and C2H4 in Pluto's atmosphere. We also present evidence for weak airglow emissions.

Kuiper Belt Objects Along the Pluto Express Path

NASA Technical Reports Server (NTRS)

Jewitt, David

1999-01-01

The objective of this proposal was to mount a ground-based search for Kuiper Belt objects near the trajectory of the NASA Pluto Express spacecraft. The high density of Kuiper Belt objects established from work on Mauna Kea makes it probable that one or more bodies can be visited by Pluto Express after its encounter with Pluto. The work was funded during its first year through NASA HQ. The second year was funded through Goddard. The third year was never funded.

Developer Initiation and Social Interactions in OSS: A Case Study of the Apache Software Foundation

DTIC Science & Technology

2014-08-01

public interaction with the Apache Pluto community is on the mailing list in August 2006: Hello all, I’am John from the University [...], we are...developing the Prototype for the JSR 286. I hope that we can discuss the code [...] we have made and then develop new code for Pluto together [...], referring...to his and some of his fellow student’s intentions to contribute to Pluto . John gets the attention of Pluto committers and is immediately welcomed as

The New Horizons Radio Science Experiment: Expected Performance in Measurements of Pluto's Atmospheric Structure, Surface Pressure, and Surface Temperature

NASA Astrophysics Data System (ADS)

Hinson, D. P.; Linscott, I.; Woods, W. W.; Tyler, G. L.; Bird, M. K.; Paetzold, M.; Strobel, D. F.

2014-12-01

The New Horizons (NH) payload includes a Radio Science Experiment (REX) for investigating key characteristics of Pluto and Charon during the upcoming flyby in July 2015. REX flight equipment augments the NH radio transceiver used for spacecraft communications and tracking. The REX hardware implementation requires 1.6 W and 160 g. This presentation will focus on the final design and the predicted performance of two high-priority observations. First, REX will receive signals from a pair of 70-m antennas on Earth - each transmitting 20 kW at 4.2-cm wavelength - during a diametric radio occultation by Pluto. The data recorded by REX will reveal the surface pressure, the temperature structure of the lower atmosphere, and the surface radius. Second, REX will measure the thermal emission from Pluto at 4.2-cm wavelength during two linear scans across the disk at close range when both the dayside and the nightside are visible, allowing the surface temperature and its spatial variations to be determined. Both scans extend from limb to limb with a resolution of about 10 pixels; one bisects Pluto whereas the second crosses the winter pole. We will illustrate the capabilities of REX by reviewing the method of analysis and the precision achieved in a lunar occultation observed by New Horizons in May 2011. Re-analysis of radio occultation measurements by Voyager 2 at Triton is also under way. More generally, REX objectives include a radio occultation search for Pluto's ionosphere; examination of Charon through both radio occultation and radiometry; a search for a radar echo from Pluto's surface; and improved knowledge of the Pluto system mass and the Pluto-Charon mass ratio from a combination of two-way and one-way Doppler frequency measurements.

(abstract) Student Involvement in the Pluto Mission

NASA Technical Reports Server (NTRS)

Weinstein, Stacy

1994-01-01

The Pluto Fast Flyby mission development baseline consists of 2 identical spacecraft (120 - 165 kg) to be launched to Pluto/ Charon in the late 1990s. These spacecraft are intended to fly by Pluto and Charon in order to perform various remote-sensing scientific investigations and have a mission development cost less than $400M (FY92$) through launch plus 30 days. The Pluto team is committed to involving students in all areas of mission development and operations. In November 1992, the Pluto team sent a request for information to industry and universities looking for ways to lower the mass and cost of the mission. A number of universities responded with creative and promising technological developments. In addition to contracts with industry and other federal labs, contracts were signed with schools which allowed students to apply their research, enabling the Pluto team to use valuable resources on a variety of advanced technology endeavors. Perhaps the most exciting aspect of these investigations was that the deliverables that the students produced were not just final reports, but actual prototype hardware complete with write-ups on lessons learned in machining, programming, and design. Another exciting development was a prototype adapter competition in which 7 universities competed to design, build, and test their idea of a lightweight spacecraft-propulsion stack adapter. Georgia Tech won with an innovative dodecahedron composite lattice cone. Other students from other universities were involved as well. All in all, over 40 students from 20 different colleges made significant contributions to the Pluto Fast Flyby mission development through their efforts. This paper will give an overview of Pluto student involvement, the technologies which they examined, and useful results for the mission.

Mapping the stability region of the 3:2 Neptune-Pluto resonance

NASA Technical Reports Server (NTRS)

Levison, H. F.; Stern, S. A.

1993-01-01

Pluto and Charon are most likely the remnants of a large number of objects that existed in the Uranus-Neptune region at early epochs of the solar system. Numerical integrations have shown that, in general, such objects were ejected from the planetary region on timescales of approximately 10(exp 7) years after Neptune and Uranus reached their current masses. It is thought that the Pluto-Charon system survived to current times without being dynamically removed in this way because it is trapped in a set of secular and mean motion resonances with Neptune. The best-known Pluto-Neptune orbit coupling is the 3:2 mean motion resonance discovered almost 30 years ago by C. Cohen and E. Hubbard. These workers showed that the resonance angle, delta is equivalent to 3(lambda(sub P)) - 2(lambda(sub N)) - omega-bar(sub P) where omega-bar(sub P) is the longitude of perihelion of the Pluto-Charon system, and lambda(sub N) and lambda(sub P) are the mean longitude of Neptune and Pluto-Charon respectively, librates about 180 deg with an amplitude, A(sub delta), of 76 deg. A numerical simulation project to map out the stability region of the 3:2 resonance is reported. The results of these simulations are important to understanding whether Pluto's long-term heliocentric stability requires only the 3:2 resonance, or whether it instead requires one or more of the other Pluto-Neptune resonances. Our study also has another important application. By investigating stability timescales as a function of orbital elements, we gain insight into the fraction of orbital phase space which the stable 3:2 resonance occupies. This fraction is directly related to the probability that the Pluto-Charon system (and possibly other small bodies) could have been captured into this resonance.

Surface compositions across Pluto and Charon.

PubMed

Grundy, W M; Binzel, R P; Buratti, B J; Cook, J C; Cruikshank, D P; Dalle Ore, C M; Earle, A M; Ennico, K; Howett, C J A; Lunsford, A W; Olkin, C B; Parker, A H; Philippe, S; Protopapa, S; Quirico, E; Reuter, D C; Schmitt, B; Singer, K N; Verbiscer, A J; Beyer, R A; Buie, M W; Cheng, A F; Jennings, D E; Linscott, I R; Parker, J Wm; Schenk, P M; Spencer, J R; Stansberry, J A; Stern, S A; Throop, H B; Tsang, C C C; Weaver, H A; Weigle, G E; Young, L A

2016-03-18

The New Horizons spacecraft mapped colors and infrared spectra across the encounter hemispheres of Pluto and Charon. The volatile methane, carbon monoxide, and nitrogen ices that dominate Pluto's surface have complicated spatial distributions resulting from sublimation, condensation, and glacial flow acting over seasonal and geological time scales. Pluto's water ice "bedrock" was also mapped, with isolated outcrops occurring in a variety of settings. Pluto's surface exhibits complex regional color diversity associated with its distinct provinces. Charon's color pattern is simpler, dominated by neutral low latitudes and a reddish northern polar region. Charon's near-infrared spectra reveal highly localized areas with strong ammonia absorption tied to small craters with relatively fresh-appearing impact ejecta. Copyright © 2016, American Association for the Advancement of Science.

The Surface Age of Sputnik Planum, Pluto, Must Be Less than 10 Million Years.

PubMed

Trilling, David E

2016-01-01

Data from the New Horizons mission to Pluto show no craters on Sputnik Planum down to the detection limit (2 km for low resolution data, 625 m for high resolution data). The number of small Kuiper Belt Objects that should be impacting Pluto is known to some degree from various astronomical surveys. We combine these geological and telescopic observations to make an order of magnitude estimate that the surface age of Sputnik Planum must be less than 10 million years. This maximum surface age is surprisingly young and implies that this area of Pluto must be undergoing active resurfacing, presumably through some cryo-geophysical process. We discuss three possible resurfacing mechanisms and the implications of each one for Pluto's physical properties.

The PLUTO plastidial nucleobase transporter also transports the thiamin precursor hydroxymethylpyrimidine

PubMed Central

Beaudoin, Guillaume A.W.; Johnson, Timothy S.; Hanson, Andrew D.

2018-01-01

In plants, the hydroxymethylpyrimidine (HMP) and thiazole precursors of thiamin are synthesized and coupled together to form thiamin in plastids. Mutants unable to form HMP can be rescued by exogenous HMP, implying the presence of HMP transporters in the plasma membrane and plastids. Analysis of bacterial genomes revealed a transporter gene that is chromosomally clustered with thiamin biosynthesis and salvage genes. Its closest Arabidopsis homolog, the plastidic nucleobase transporter (PLUTO), is co-expressed with several thiamin biosynthetic enzymes. Heterologous expression of PLUTO in Escherichia coli or Saccharomyces cerevisiae increased sensitivity to a toxic HMP analog, and disrupting PLUTO in an HMP-requiring Arabidopsis line reduced root growth at low HMP concentrations. These data implicate PLUTO in plastidial transport and salvage of HMP. PMID:29507060

Pluto and Charon in Color: Barycentric View Animation

NASA Image and Video Library

2015-06-11

The first color movies from NASA's New Horizons mission show Pluto and its largest moon, Charon, and the complex orbital dance of the two bodies, known as a double planet. A near-true color movie was assembled from images made in three colors -- blue, red and near-infrared -- by the Multispectral Visible Imaging Camera on the instrument known as Ralph. The images were taken on nine different occasions from May 29-June 3, 2015. The movie is barycentric, meaning that both Pluto and Charon are shown in motion around the binary's barycenter -- the shared center of gravity between the two bodies as they do a planetary jig. Because Pluto is much more massive than Charon, the barycenter (marked by a small "x" in the movie) is much closer to Pluto than to Charon. Looking closely at the images in this movie, one can detect a regular shift in Pluto's brightness-due to the brighter and darker terrains on its differing faces. http://photojournal.jpl.nasa.gov/catalog/PIA19688

Haze heats Pluto's atmosphere yet explains its cold temperature.

PubMed

Zhang, Xi; Strobel, Darrell F; Imanaka, Hiroshi

2017-11-15

Pluto's atmosphere is cold and hazy. Recent observations have shown it to be much colder than predicted theoretically, suggesting an unknown cooling mechanism. Atmospheric gas molecules, particularly water vapour, have been proposed as a coolant; however, because Pluto's thermal structure is expected to be in radiative-conductive equilibrium, the required water vapour would need to be supersaturated by many orders of magnitude under thermodynamic equilibrium conditions. Here we report that atmospheric hazes, rather than gases, can explain Pluto's temperature profile. We find that haze particles have substantially larger solar heating and thermal cooling rates than gas molecules, dominating the atmospheric radiative balance from the ground to an altitude of 700 kilometres, above which heat conduction maintains an isothermal atmosphere. We conclude that Pluto's atmosphere is unique among Solar System planetary atmospheres, as its radiative energy equilibrium is controlled primarily by haze particles instead of gas molecules. We predict that Pluto is therefore several orders of magnitude brighter at mid-infrared wavelengths than previously thought-a brightness that could be detected by future telescopes.

Flight set 360L007 (STS-33) insulation component. Volume 3: Final release

NASA Technical Reports Server (NTRS)

Hicken, Steve

1990-01-01

Volume 3 of this postfire report deals with the insulation component of the RSRM. The report is released twice for each flight set. The interim release contract date is on or before 60 days after the last field joint or nozzle to case joint is disassembled at KSC and contain the results of the KSC visual evaluation. The data contained in Volume 3 interim release supersedes the insulation data presented in the KSC 10 day report. The final release contract data is on or before 60 days after the last factory joint is disassembled at the Clearfield H-7 facility and contains the results of all visual evaluations and a thermal safety factor analysis. The data contained in the Volume 3 final release supersedes the interim release and the insulation data presented in the Clearfield 10 day report.

The New Horizons Radio Science Experiment: Performance and Measurements of Pluto's Atmospheric Structure, Surface Pressure, and Surface Temperature

NASA Astrophysics Data System (ADS)

Linscott, I.; Hinson, D. P.; Bird, M. K.; Stern, A.; Weaver, H. A., Jr.; Olkin, C.; Young, L. A.; Ennico Smith, K.

2015-12-01

The New Horizons (NH) spacecraft payload contained the Radio Science Experiment (REX) for determining key characteristics of Pluto and Charon during the July 14, 2015, flyby of the Pluto/Charon system. The REX flight equipment augments the NH X-band radio transceiver by providing a high precision, narrow band recording of high power uplink transmissions from Earth stations, as well as a record of broadband radiometric power. This presentation will review the performance and initial results of two high- priority observations. First, REX received two pair of 20-kW signals, one pair per polarization, transmitted from the DSN at 4.2-cm wavelength during a diametric radio occultation by Pluto. REX recorded these uplink signals and determined precise measurement of the surface pressure, the temperature structure of the lower atmosphere, and the surface radius of Pluto. The ingress portion of one polarization was played back from the spacecraft in July and processed to obtain the pressure and temperature structure of Pluto's atmosphere. Second, REX measured the thermal emission from Pluto at 4.2- cm wavelength during two linear scans across the disk at close range when both the dayside and the night side are visible. Both scans extend from limb to limb with a resolution of one-tenth Pluto's disk and temperature resolution of 0.1 K. Occultation and radiometric temperature results presented here will encompass additional data scheduled for playback in September.

Mirages and the nature of Pluto's atmosphere

NASA Technical Reports Server (NTRS)

Stansberry, J. A.; Lunine, J. I.; Hubbard, W. B.; Yelle, R. V.; Hunten, D. M.

1994-01-01

We present model occultation lightcurves demonstrating that a strong thermal inversion layer at the base of Pluto's stratosphere can reproduce the minimum flux measured by the Kuiper Airborne Observatory (KAO) during the 1988 occultation of a star by Pluto. The inversion layer also forms the occultation equivalent of a mirage at a radius of 1198 km, which is capable of hiding tropospheres of significant depth. Pluto's surface lies below 1198 km, its radius depending on the depth of the troposphere. We begin by computing plausible temperature structures for Pluto's lower atmosphere, constrained by a calculation of the temperature of the atmosphere near the surface. We then trace rays from the occulted star through the model atmosphere, computing the resultant bending of the ray. Model light curves are obtained by summing the contribution of individual rays within the shadow of Pluto on Earth. We find that we can reproduce the KAO lightcurve using model atmospheres with a temperature inversion and no haze. We have explored models with tropospheres as deep as 40 km (implying a Pluto radius of 1158 km) that reproduce the suite of occultation data. Deeper tropospheres can be fitted to the data, but the mutual event radius of 1150 km probably provides a lower bound. If Pluto has a shallow or nonexistent troposphere, its density is consistent with formation in the solar nebula with modest water loss due to impact ejection. If the troposhere is relatively deep, implying a smaller radius and larger density, significant amounts of water loss are required.

18. Photocopy of photograph. VIEW WITHIN POSTMORTEM CELL OF MANIPULATOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

18. Photocopy of photograph. VIEW WITHIN POST-MORTEM CELL OF MANIPULATOR ARMS BEING USED TO MOVE METAL BARS FROM ONE LOCATION TO ANOTHER. Photographer unknown, ca. 1965, original photograph and negative on file at the Remote Sensing Laboratory, Department of Energy, Nevada Operations Office. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

19. Photocopy of photograph. VIEW OF WORKER MANIPULATING SMALL GLASS ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

19. Photocopy of photograph. VIEW OF WORKER MANIPULATING SMALL GLASS OBJECTS IN THE HOT BAY WITH MANIPULATOR ARMS AT WORK STATION E-2. Photographer unknown, ca. 1969, original photograph and negative on file at the Remote Sensing Laboratory, Department of Energy, Nevada Operations Office. - Nevada Test Site, Engine Maintenance Assembly & Disassembly Facility, Area 25, Jackass Flats, Mercury, Nye County, NV

36. INTERIOR VIEW TO THE NORTHWEST OF THE SECOND FLOOR ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

36. INTERIOR VIEW TO THE NORTHWEST OF THE SECOND FLOOR CORRIDOR ON THE EAST SIDE OF THE DISASSEMBLY BAY. A VIEWING AND WORK STATION AND ENTRANCE TO THE CONTROL ROOM ARE ON THE WEST SIDE OF THE CORRIDOR. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

East Europe Report.

DTIC Science & Technology

1986-12-05

and road building equipment manufactured by the Martin Heavy Engineering Plants, economic production unit [VHJ], one of our major suppliers, the...equipped with health care facilities, their major advantage is that they can be rapidly assembled and disassembled even under demanding field conditions... major crude oil pipelines. In the Seventh 5-Year Plan the Czechoslovak Freight Car Works, concern enterprise, in Poprad manufactured numerous BMPNS

ARC: A compact, high-field, disassemblable fusion nuclear science facility and demonstration power plant

NASA Astrophysics Data System (ADS)

Sorbom, Brandon; Ball, Justin; Palmer, Timothy; Mangiarotti, Franco; Sierchio, Jennifer; Bonoli, Paul; Kasten, Cale; Sutherland, Derek; Barnard, Harold; Haakonsen, Christian; Goh, Jon; Sung, Choongki; Whyte, Dennis

2014-10-01

The Affordable, Robust, Compact (ARC) reactor conceptual design aims to reduce the size, cost, and complexity of a combined Fusion Nuclear Science Facility (FNSF) and demonstration fusion pilot power plant. ARC is a 270 MWe tokamak reactor with a major radius of 3.3 m, a minor radius of 1.1 m, and an on-axis magnetic field of 9.2 T. ARC has Rare Earth Barium Copper Oxide (REBCO) superconducting toroidal field coils with joints to allow disassembly, allowing for removal and replacement of the vacuum vessel as a single component. Inboard-launched current drive of 25 MW LHRF power and 13.6 MW ICRF power is used to provide a robust, steady state core plasma far from disruptive limits. ARC uses an all-liquid blanket, consisting of low pressure, slowly flowing Fluorine Lithium Beryllium (FLiBe) molten salt. The liquid blanket acts as a working fluid, coolant, and tritium breeder, and minimizes the solid material that can become activated. The large temperature range over which FLiBe is liquid permits blanket operation at 800-900 K with single phase fluid cooling and allows use of a high-efficiency Brayton cycle for electricity production in the secondary coolant loop.

Generation of control sequences for a pilot-disassembly system

NASA Astrophysics Data System (ADS)

Seliger, Guenther; Kim, Hyung-Ju; Keil, Thomas

2002-02-01

Closing the product and material cycles has emerged as a paradigm for industry in the 21st century. Disassembly plays a key role in a life cycle economy since it enables the recovery of resources. A partly automated disassembly system should adapt to a large variety of products and different degrees of devaluation. Also the amounts of products to be disassembled can vary strongly. To cope with these demands an approach to generate on-line disassembly control sequences will be presented. In order to react on these demands the technological feasibility is considered within a procedure for the generation of disassembly control sequences. Procedures are designed to find available and technologically feasible disassembly processes. The control system is formed by modularised and parameterised control units in the cell level within the entire control architecture. In the first development stage product and process analyses at the sample product washing machine were executed. Furthermore a generalized disassembly process was defined. Afterwards these processes were structured in primary and secondary functions. In the second stage the disassembly control at the technological level was investigated. Factors were the availability of the disassembly tools and the technological feasibility of the disassembly processes within the disassembly system. Technical alternative disassembly processes are determined as a result of availability of the tools and technological feasibility of processes. The fourth phase was the concept for the generation of the disassembly control sequences. The approach will be proved in a prototypical disassembly system.

Miniatue Propulsion Components for the Pluto Fast Flyby Spacecraft

NASA Technical Reports Server (NTRS)

Morash, D. H.; Strand, L.

1994-01-01

Pluto is the only planet in our solar system not yet visited by our spacecraft. Recent observations through the Hubble Space Telescope have given us a glimpse of Pluto and it's moon Charon, but their small size and immense distance from earth have preserved their mystery.

The Exploration of the Pluto System by New Horizons

NASA Astrophysics Data System (ADS)

Weaver, Harold; Stern, S. Alan

2016-07-01

The New Horizons (NH) mission was selected by NASA in November 2001 to conduct the first in situ reconnaissance of Pluto and the Kuiper belt. The NH spacecraft was launched on 2006 January 19, received a gravity assist from Jupiter during closest approach on 2007 February 28, and flew 12,500 km above Pluto's surface on 2015 July 14. NH carried a sophisticated suite of seven scientific instruments, altogether weighing less than 30 kg and drawing less than 30 W of power, that includes panchromatic and color imagers, ultraviolet and infrared spectral imagers, a radio science package, plasma and charged particle sensors, and a dust counting experiment. The NH flyby of the Pluto system executed flawlessly, providing unprecedented detail on the Pluto-Charon binary and Pluto's four small moons (Styx, Nix, Kerberos, and Hydra, in order of their orbital distance from Pluto). Pluto's surface displays diverse landforms, terrain ages, albedos, colors, and composition gradients. Evidence is found for a water-ice crust, geologically young surface units, surface ice convection, wind streaks, volatile transport, and glacial flow. NH discovered trace hydrocarbons in Pluto's atmosphere, multiple global haze layers, and a surface pressure near 10 microbars. Pluto's diverse surface geology and long term activity raise fundamental questions about how small planets remain active many billions of years (Gyr) after formation. Charon displays tectonics, evidence for a heterogeneous crustal composition, and a puzzling giant hood of dark material covering its North Pole. Crater density statistics for Charon's surface give a crater retention age of 4-4.5 Ga, indicating that Charon's geological evolution largely ceased early in its history. Nix and Hydra have high albedos suggestive of H2O-ice covered surfaces. Crater densities on Nix and Hydra indicate surface ages > 4 Ga. All the small satellites have highly elongated shapes and are rotating much faster then synchronous with their orbital periods, with rotational poles clustered near the Pluto-Charon orbital plane. The NH spacecraft remains healthy and was targeted toward the flyby of a small (~30-40 km diameter) KBO in late-2015, enabling the study of an object (2014 MU69) in a completely different dynamical class (cold classical) than Pluto, if NASA approves an Extended Mission phase. The proposed Extended Mission would also include observations of more than 20 other KBOs at resolutions and geometries not feasible from Earth, and studies of the heliospheric plasma, neutral H and He, and the dust environment out to 50 AU from the Sun.

A giant impact origin of Pluto-Charon.

PubMed

Canup, Robin M

2005-01-28

Pluto and its moon, Charon, are the most prominent members of the Kuiper belt, and their existence holds clues to outer solar system formation processes. Here, hydrodynamic simulations are used to demonstrate that the formation of Pluto-Charon by means of a large collision is quite plausible. I show that such an impact probably produced an intact Charon, although it is possible that a disk of material orbited Pluto from which Charon later accumulated. These findings suggest that collisions between 1000-kilometer-class objects occurred in the early inner Kuiper belt.

Kuiper Belt Objects Along the Pluto Express Path

NASA Technical Reports Server (NTRS)

Jewitt, David C.

1998-01-01

The science objective of this work was to identify objects in the Kuiper Belt which will, in the 5 years following Pluto encounter, be close to the flight path of NASA's Pluto-Kuiper Express. Currently, launch is scheduled for 2004 with a flight time of about 1 decade. Early identification of post-Pluto targets is important for mission design and orbit refinement. An object or objects close enough to the flight path can be visited and studied at high resolution, using only residual gas in the thrusters to affect a close encounter.

Hemispherical Pluto and Charon Color Composition From New Horizons

NASA Technical Reports Server (NTRS)

Ennico, K.; Parker, A.; Howett, C. A. J.; Olkin, C. B.; Spencer, J. R.; Grundy, W. M.; Reuter, D. E.; Cruikshank, D. P.; Binzel, R. P.; Buie, M. W.;

New Horizons at Pluto

NASA Technical Reports Server (NTRS)

2007-01-01

Artist's concept of the New Horizons spacecraft as it approaches Pluto and its largest moon, Charon, in July 2015. The craft's miniature cameras, radio science experiment, ultraviolet and infrared spectrometers and space plasma experiments will characterize the global geology and geomorphology of Pluto and Charon, map their surface compositions and temperatures, and examine Pluto's atmosphere in detail. The spacecraft's most prominent design feature is a nearly 7-foot (2.1-meter) dish antenna, through which it will communicate with Earth from as far as 4.7 billion miles (7.5 billion kilometers) away.

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

An audience member asks the panelists a question at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. Scientists discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

On the origin of Triton and Pluto

NASA Technical Reports Server (NTRS)

Mckinnon, W. B.

1984-01-01

Lyttleton's (1936) hypothesis that Triton and Pluto originated as adjacent prograde satellites of Neptune is evaluated, and it is shown that with the presently accepted masses of Triton and Pluto-Charon, the momentum and energy exchange required to set Triton on a retrograde orbit is impossible. The Pluto-Charon system could not have acquired its present angular momentum state during an ejection event unless a physical collision was involved, which is quite unlikely. The simplest hypothesis is that Triton and Pluto are independent representatives of large outer solar system planetesimals. Triton is simply captured, with spectacular consequences that include runaway melting of interior ices and release to the surface of clathrated CH4, CO, and N2. Condensed remnants of this protoatmosphere could account for features in Triton's unique spectrum.

On the Origin of Triton and Pluto

NASA Technical Reports Server (NTRS)

Mckinnon, W. B.

1985-01-01

Lyttleton's (1936) hypothesis that Triton and Pluto originated as adjacent prograde satellites of Neptune is evaluated, and it is shown that with the presently accepted masses of Triton and Pluto-Charon, the momentum and energy exchange required to sell Triton on a retrograde orbit is impossible. The Pluto-Charon system could not have acquired its present angular momentum state during an ejection event unless a physical collision was involved, which is quite unlikely. The simplest hypothesis is that Triton and Pluto are independent representatives of large outer solar system planetesimals. Triton is simply captured, with spectacular consequences that include runaway melting of interior ices and release to the surface of clathrated CH4, CO, and N2. Condensed remnants of this protoatmosphere could account for features in Triton's unique spectrum.

The PLUTO plastidial nucleobase transporter also transports the thiamin precursor hydroxymethylpyrimidine.

PubMed

Beaudoin, Guillaume A W; Johnson, Timothy S; Hanson, Andrew D

2018-04-27

In plants, the hydroxymethylpyrimidine (HMP) and thiazole precursors of thiamin are synthesized and coupled together to form thiamin in plastids. Mutants unable to form HMP can be rescued by exogenous HMP, implying the presence of HMP transporters in the plasma membrane and plastids. Analysis of bacterial genomes revealed a transporter gene that is chromosomally clustered with thiamin biosynthesis and salvage genes. Its closest Arabidopsis homolog, the plastidic nucleobase transporter (PLUTO), is co-expressed with several thiamin biosynthetic enzymes. Heterologous expression of PLUTO in Escherichia coli or Saccharomyces cerevisiae increased sensitivity to a toxic HMP analog, and disrupting PLUTO in an HMP-requiring Arabidopsis line reduced root growth at low HMP concentrations. These data implicate PLUTO in plastidial transport and salvage of HMP. © 2018 The Author(s).

FIRST ULTRAVIOLET REFLECTANCE SPECTRA OF PLUTO AND CHARON BY THE HUBBLE SPACE TELESCOPE COSMIC ORIGINS SPECTROGRAPH: DETECTION OF ABSORPTION FEATURES AND EVIDENCE FOR TEMPORAL CHANGE

DOE Office of Scientific and Technical Information (OSTI.GOV)

Stern, S. A.; Spencer, J. R.; Shinn, A.

We have observed the mid-UV spectra of both Pluto and its large satellite, Charon, at two rotational epochs using the Hubble Space Telescope (HST) Cosmic Origins Spectrograph (COS) in 2010. These are the first HST/COS measurements of Pluto and Charon. Here we describe the observations and our reduction of them, and present the albedo spectra, average mid-UV albedos, and albedo slopes we derive from these data. These data reveal evidence for a strong absorption feature in the mid-UV spectrum of Pluto; evidence for temporal change in Pluto's spectrum since the 1990s is reported, and indirect evidence for a near-UV spectralmore » absorption on Charon is also reported.« less

The subsurface of Pluto from submillimetre observations

NASA Astrophysics Data System (ADS)

Greaves, J. S.; Whitelaw, A. C. M.; Bendo, G. J.

2015-04-01

Surface areas on Pluto change in brightness and colour, at optical to infrared wavelengths, over time-scales as short as years. The subsurface contains a reservoir of frozen volatiles, but little is known about it because Pluto is out of reach for cm-radar. Here we present a 0.85 mm wavelength light curve of the Pluto system, from archival data taken in 1997 August with the SCUBA (Submillimetre Common-User Bolometer Array) camera on the James Clerk Maxwell Telescope (JCMT). This wavelength probes for the first time to just below the skin depth of thermal changes over Pluto's day. The light curve differs significantly from counterparts in the mid- to far-infrared, in a longitude range that is optically dark on Pluto's surface. An estimate from Herschel of the 0.5 mm flux in 2012 is comparable to the mean 0.45 mm flux from SCUBA in 1997, suggesting that layers centimetres below the surface have not undergone any gross temperature change. The longitudes that are relatively submillimetre-faint could have a different emissivity, perhaps with a subsurface layer richer in nitrogen or methane ices than at the surface. The Radio Science Experiment (REX) instrument on New Horizons may be able to constrain physical properties deeper down, as it looks back on Pluto's nightside after the 2015 July flyby.

Determination of the System Mass and the Individual Masses of Pluto and Charon from New Horizons Radio Tracking

NASA Astrophysics Data System (ADS)

Hahn, M.; Paetzold, M.; Andert, T.; Bird, M. K.; Tyler, G. L.; Hinson, D. P.; Linscott, I.; Stern, A.; Weaver, H. A., Jr.; Young, L. A.; Ennico Smith, K.; Olkin, C.

2016-12-01

One objective of the New Horizons Radio Science Experiment REX is the direct determination of the system mass and the individual masses of Pluto and Charon. About four weeks of two-way radio tracking centered around the closest approach of New Horizons to the Pluto system were processed. Major problems during the processing were the changes in spacecraft attitude by thrusters which applied extra Δv to the spacecraft motion masking partially the continuously perturbed motion caused by the attracting forces of the Pluto system members. The times of the spacecraft thruster activity are known but the applied Δv magnitude needed to be specifically adjusted. No two-way tracking was available during the flyby day on 14th July but slots of the REX one-way uplink observations cover the most important time near closest approach, these are for example the Pluto and Charon Earth occultation entries and exits. The REX data during the flyby day allowed to extract the individual masses of Pluto and Charon from the system mass at high precision. The relative errors of the mass determinations are below 0.02% and 0.2%, respectively. The masses of the 4 small satellites in the Pluto system could not be resolved.

Pluto's Nonvolatile Chemical Compounds

NASA Astrophysics Data System (ADS)

Grundy, William M.; Binzel, Richard; Cook, Jason C.; Cruikshank, Dale P.; Dalle Ore, Cristina M.; Earle, Alissa M.; Ennico, Kimberly; Jennings, Donald; Howett, Carly; Kaiser, Ralf-Ingo; Linscott, Ivan; Lunsford, A. W.; Olkin, Catherine B.; Parker, Alex Harrison; Parker, Joel Wm.; Philippe, Sylvain; Protopapa, Silvia; Quirico, Eric; Reuter, D. C.; Schmitt, Bernard; Singer, Kelsi N.; Spencer, John R.; Stansberry, John A.; Stern, S. Alan; Tsang, Constantine; Verbiscer, Anne J.; Weaver, Harold A.; Weigle, G. E.; Young, Leslie

2016-10-01

Despite the migration of Pluto's volatile ices (N2, CO, and CH4) around the surface on seasonal timescales, the planet's non-volatile materials are not completely hidden from view. They occur in a variety of provinces formed over a wide range of timescales, including rugged mountains and chasms, the floors of mid-latitude craters, and an equatorial belt of especially dark and reddish material typified by the informally named Cthulhu Regio. NASA's New Horizons probe observed several of these regions at spatial resolutions as fine as 3 km/pixel with its LEISA imaging spectrometer, covering wavelengths from 1.25 to 2.5 microns. Various compounds that are much lighter than the tholin-like macromolecules responsible for the reddish coloration, but that are not volatile at Pluto surface temperatures such as methanol (CH3OH) and ethane (C2H6) have characteristic absorption bands within LEISA's wavelength range. This presentation will describe their geographic distributions and attempt to constrain their origins. Possibilities include an inheritance from Pluto's primordial composition (the likely source of H2O ice seen on Pluto's surface) or ongoing production from volatile precursors through photochemistry in Pluto's atmosphere or through radiolysis on Pluto's surface. New laboratory data inform the analysis.This work was supported by NASA's New Horizons project.

KSC-05pd2323

NASA Image and Video Library

2005-10-11

KENNEDY SPACE CENTER, FLA. - Inside the mobile service tower on Launch Complex 41 at Cape Canaveral Air Force Station in Florida, workers oversee the lowering of the Lockheed Martin Atlas V Centaur stage (above) toward the first stage. The two stages will be mated. The Atlas V is the launch vehicle for the New Horizons spacecraft. New Horizons will make the first reconnaissance of Pluto and its moon, Charon - a "double planet" and the last planet in our solar system to be visited by spacecraft. As it approaches Pluto, the spacecraft will look for ultraviolet emission from Pluto's atmosphere and make the best global maps of Pluto and Charon in green, blue, red and a special wavelength that is sensitive to methane frost on the surface. It will also take spectral maps in the near infrared, telling the science team about Pluto's and Charon's surface compositions and locations and temperatures of these materials. When the spacecraft is closest to Pluto or its moon, it will take close-up pictures in both visible and near-infrared wavelengths. The mission will then visit one or more objects in the Kuiper Belt region beyond Neptune. New Horizons is scheduled to launch in January 2006, swing past Jupiter for a gravity boost and scientific studies in February or March 2007, and reach Pluto and Charon in July 2015.

Where is the Geophysical Evidence for the Giant Impact Origin of the Pluto System?

NASA Astrophysics Data System (ADS)

McKinnon, W. B.; Singer, K. N.; Nimmo, F.; Spencer, J. R.; Young, L. A.; Weaver, H. A., Jr.; Stern, S. A.

2016-12-01

Prior to the New Horizons flyby of the Pluto system, it was anticipated that both Pluto and Charon might show geological or geophysical evidence of the giant impact thought responsible for the formation of Charon and the smaller satellites. Although dynamical and compositional evidence still supports the giant impact model (McKinnon et al., submitted to Icarus), the question remains as to whether the geology of Pluto or Charon records evidence of this cataclysm. The collision speed and energy were most likely not large enough to melt all the ices in the precursor bodies, so surviving geological evidence is not out of the question. Specifically, Pluto post-impact should have been rapidly rotating (with a period as short as 5-6 hr) and highly distorted; Charon under most circumstances would have rapidly despun but have been a highly distorted triaxial body. The tidal evolution end state for both is close to spherical, but fossil figures were anticipated, which in addition to providing direct evidence for post-impact tidal evolution, would provide important clues to thermal and structural evolution. For Pluto, McKinnon and Singer (DPS 2014, abs. 419.07) predicted a flattening >1% (radii differences >10 km) for a strengthless icy lithosphere and an unrelaxed rock core. For a fully relaxed core, they predicted a >2-3 km fossil bulge supported by icy lithospheric strength (corresponding to a minimum past lithosphere thickness of 50 km). New Horizons image analyses have limited any oblateness for Pluto to 0.6% (Nimmo et al., Icarus, in press), which corresponds to <7 km flattening. So Pluto may yet possess a geophysically meaningful oblateness, only one not yet directly detectable (moreover, in order to be consistent with the observations, Pluto's rock core either completed its formation post-spindown, or was too weak to support much non-hydrostatic topography). Such an equator-to-pole surface elevation difference, even a subtle one, could express itself through control of Pluto's zonal albedo pattern (i.e., dark, reddish Cthulhu Regio, Krun and other Macula are all equatorial [names are informal]). Even for a completely relaxed shape, the tectonic effects on Pluto's surface should be manifest. There is a rich variety of tectonic expression, but no obvious match to classic predicted tectonic despinning patterns.

Detailed Astrometric Analysis of Pluto

NASA Astrophysics Data System (ADS)

ROSSI, GUSTAVO B.; Vieira-Martins, R.; Camargo, J. I.; Assafin, M.

2013-05-01

Abstract (2,250 Maximum Characters): Pluto is the main representant of the transneptunian objects (TNO's), presenting some peculiarities such as an atmosphere and a satellite system with 5 known moons: Charon, discovered in 1978, Nix and Hydra, in 2006, P4 in 2011 and P5 in 2012. Until the arrival of the New Horizons spacecraft to this system (july 2015), stellar occultations are the most efficient method, from the ground, to know physical and dinamical properties of this system. In 2010, it was evident a drift in declinations (about 20 mas/year) comparing to the ephemerides. This fact motivated us to remake the reductions and analysis of a great set of our observations at OPD/LNA, in a total of 15 years. The ephemerides and occultations results was then compared with the astrometric and photometric reductions of CCD images of Pluto (around 6500 images). Two corrections were used for a refinement of the data set: diferential chromatic refraction and photocenter. The first is due to the mean color of background stars beeing redder than the color of Pluto, resulting in a slightly different path of light through the atmosphere (that may cause a difference in position of 0.1”). It became more evident because Pluto is crossing the region of the galactic plane. The photocenter correction is based on two gaussians curves overlapped, with different hights and non-coincident centers, corresponding to Pluto and Charon (since they have less than 1” of angular separation). The objective is to separate these two gaussian curves from the observed one and find the right position of Pluto. The method is strongly dependent of the hight of each of the gaussian curves, related to the respective albedos of charon and Pluto. A detailed analysis of the astrometric results, as well a comparison with occultation results was made. Since Pluto has an orbital period of 248,9 years and our interval of observation is about 15 years, we have around 12% of its observed orbit and also, our observations were made when Pluto was near its periapsis. With the corrections made, the ephemeris, when recalculated, shall not present sistematic drifts near the temporal interval in wich contains our observational data, allowing the determination of local adjustments at the Pluto orbit.

KSC-05pd2547

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - In NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, Boeing workers attach a crane to the top of the cover surrounding the third stage, or upper stage, for the New Horizons spacecraft. The third stage is a Boeing STAR 48 solid-propellant kick motor. The launch vehicle for New Horizons is the Atlas V rocket, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11, and fly through the Pluto system as early as summer 2015.

Addendum to the Closure Report for Corrective Action Unit 113: Area 25 R-MAD Facility, Nevada National Security Site, Nevada

DOE Office of Scientific and Technical Information (OSTI.GOV)

NSTec Environmental Restoration

2011-02-24

This addendum to the Closure Report for Corrective Action Unit 113: Area 25, Reactor Maintenance, Assembly, and Disassembly Facility, Building 3110, Nevada Test Site, Nevada, DOE/NV--891-VOL I-Rev. 1, dated July 2003, provides details of demolition, waste disposal, and use restriction (UR) modification for Corrective Action Unit 113, Area 25 R-MAD Facility. Demolition was completed on July 15, 2010, when the last of the building debris was disposed. Final field activities were concluded on August 30, 2010, after all equipment was demobilized and UR signs were posted. This work was funded by the American Recovery and Reinvestment Act.

The rapid formation of Sputnik Planitia early in Pluto's history.

PubMed

Hamilton, Douglas P; Stern, S A; Moore, J M; Young, L A

2016-11-30

Pluto's Sputnik Planitia is a bright, roughly circular feature that resembles a polar ice cap. It is approximately 1,000 kilometres across and is centred on a latitude of 25 degrees north and a longitude of 175 degrees, almost directly opposite the side of Pluto that always faces Charon as a result of tidal locking. One explanation for its location includes the formation of a basin in a giant impact, with subsequent upwelling of a dense interior ocean. Once the basin was established, ice would naturally have accumulated there. Then, provided that the basin was a positive gravity anomaly (with or without the ocean), true polar wander could have moved the feature towards the Pluto-Charon tidal axis, on the far side of Pluto from Charon. Here we report modelling that shows that ice quickly accumulates on Pluto near latitudes of 30 degrees north and south, even in the absence of a basin, because, averaged over its orbital period, those are Pluto's coldest regions. Within a million years of Charon's formation, ice deposits on Pluto concentrate into a single cap centred near a latitude of 30 degrees, owing to the runaway albedo effect. This accumulation of ice causes a positive gravity signature that locks, as Pluto's rotation slows, to a longitude directly opposite Charon. Once locked, Charon raises a permanent tidal bulge on Pluto, which greatly enhances the gravity signature of the ice cap. Meanwhile, the weight of the ice in Sputnik Planitia causes the crust under it to slump, creating its own basin (as has happened on Earth in Greenland). Even if the feature is now a modest negative gravity anomaly, it remains locked in place because of the permanent tidal bulge raised by Charon. Any movement of the feature away from 30 degrees latitude is countered by the preferential recondensation of ices near the coldest extremities of the cap. Therefore, our modelling suggests that Sputnik Planitia formed shortly after Charon did and has been stable, albeit gradually losing volume, over the age of the Solar System.

The rapid formation of Sputnik Planitia early in Pluto's history

NASA Astrophysics Data System (ADS)

Hamilton, Douglas P.; Stern, S. A.; Moore, J. M.; Young, L. A.; Binzel, R. P.; Buie, M. W.; Buratti, B. J.; Cheng, A. F.; Ennico, K.; Grundy, W. M.; Linscott, I. R.; McKinnon, W. B.; Olkin, C. B.; Reitsema, H. J.; Reuter, D. C.; Schenk, P.; Showalter, M. R.; Spencer, J. R.; Tyler, G. L.; Weaver, H. A.

2016-12-01

Pluto's Sputnik Planitia is a bright, roughly circular feature that resembles a polar ice cap. It is approximately 1,000 kilometres across and is centred on a latitude of 25 degrees north and a longitude of 175 degrees, almost directly opposite the side of Pluto that always faces Charon as a result of tidal locking. One explanation for its location includes the formation of a basin in a giant impact, with subsequent upwelling of a dense interior ocean. Once the basin was established, ice would naturally have accumulated there. Then, provided that the basin was a positive gravity anomaly (with or without the ocean), true polar wander could have moved the feature towards the Pluto-Charon tidal axis, on the far side of Pluto from Charon. Here we report modelling that shows that ice quickly accumulates on Pluto near latitudes of 30 degrees north and south, even in the absence of a basin, because, averaged over its orbital period, those are Pluto's coldest regions. Within a million years of Charon's formation, ice deposits on Pluto concentrate into a single cap centred near a latitude of 30 degrees, owing to the runaway albedo effect. This accumulation of ice causes a positive gravity signature that locks, as Pluto's rotation slows, to a longitude directly opposite Charon. Once locked, Charon raises a permanent tidal bulge on Pluto, which greatly enhances the gravity signature of the ice cap. Meanwhile, the weight of the ice in Sputnik Planitia causes the crust under it to slump, creating its own basin (as has happened on Earth in Greenland). Even if the feature is now a modest negative gravity anomaly, it remains locked in place because of the permanent tidal bulge raised by Charon. Any movement of the feature away from 30 degrees latitude is countered by the preferential recondensation of ices near the coldest extremities of the cap. Therefore, our modelling suggests that Sputnik Planitia formed shortly after Charon did and has been stable, albeit gradually losing volume, over the age of the Solar System.

Pluto and Charon: Ice Worlds on the Ragged Edge of the Solar System

NASA Astrophysics Data System (ADS)

Stern, Alan; Mitton, Jacqueline

1997-10-01

Rave reviews for Pluto and Charon: Ice Worlds on the Ragged Edge of the Solar System The story of the quest to understand Pluto and the resulting transformation of our concept of the diminutive planet from that of solar-system misfit to king of the Kuiper Belt is told in this book by Alan Stern and Jacqueline Mitton. Stern, a Plutophile to the core, is one of the most energetic, talented, and savvy planetary astronomers in the business today. Mitton, trained as an astronomer, is an experienced writer and editor of scientific books for nonscientists. Together they have created an immensely informative book . . . Written in an engaging and informal style, Pluto and Charon takes the reader step by step from the discovery of the ninth planet in 1930 to the current understanding of Pluto and its moon, Charon.-Sky & Telescope More than a book summarizing what we know about [the] planet, [Pluto and Charon is] about how far and how fast astronomical technology has come since 1965 . . . Stern and Mitton use the narrative of Pluto research to explain in comfortable, everyday language how such work is done . . . One of the nice touches in the book is that Stern and Mitton tell us something about each astronomer.-Astronomy Pluto and Charon presents the exploration of the ninth planet-written as a vivid historical account-for anyone with an interest in science and astronomy . . . the authors describe in simple language the methods researchers use to explore the universe and the way ever-improving instrumentation helps their knowledge advance.-Physics Today

The Icy Mountains of Pluto

NASA Image and Video Library

2015-07-15

New close-up images of a region near Pluto's equator reveal a giant surprise: a range of youthful mountains rising as high as 11,000 feet (3,500 meters) above the surface of the icy body. The mountains likely formed no more than 100 million years ago -- mere youngsters relative to the 4.56-billion-year age of the solar system -- and may still be in the process of building. That suggests the close-up region, which covers less than one percent of Pluto's surface, may still be geologically active today. The youthful age estimate is based on the lack of craters in this scene. Like the rest of Pluto, this region would presumably have been pummeled by space debris for billions of years and would have once been heavily cratered -- unless recent activity had given the region a facelift, erasing those pockmarks. Unlike the icy moons of giant planets, Pluto cannot be heated by gravitational interactions with a much larger planetary body. Some other process must be generating the mountainous landscape. The mountains are probably composed of Pluto's water-ice "bedrock." Although methane and nitrogen ice covers much of the surface of Pluto, these materials are not strong enough to build the mountains. Instead, a stiffer material, most likely water-ice, created the peaks. The close-up image was taken about 1.5 hours before New Horizons closest approach to Pluto, when the craft was 47,800 miles (770,000 kilometers) from the surface of the planet. The image easily resolves structures smaller than a mile across. http://photojournal.jpl.nasa.gov/catalog/PIA19710

Structure-Function Relationship of a Plant NCS1 Member – Homology Modeling and Mutagenesis Identified Residues Critical for Substrate Specificity of PLUTO, a Nucleobase Transporter from Arabidopsis

PubMed Central

Witz, Sandra; Panwar, Pankaj; Schober, Markus; Deppe, Johannes; Pasha, Farhan Ahmad; Lemieux, M. Joanne; Möhlmann, Torsten

2014-01-01

Plastidic uracil salvage is essential for plant growth and development. So far, PLUTO, the plastidic nucleobase transporter from Arabidopsis thaliana is the only known uracil importer at the inner plastidic membrane which represents the permeability barrier of this organelle. We present the first homology model of PLUTO, the sole plant NCS1 member from Arabidopsis based on the crystal structure of the benzyl hydantoin transporter MHP1 from Microbacterium liquefaciens and validated by molecular dynamics simulations. Polar side chains of residues Glu-227 and backbones of Val-145, Gly-147 and Thr-425 are proposed to form the binding site for the three PLUTO substrates uracil, adenine and guanine. Mutational analysis and competition studies identified Glu-227 as an important residue for uracil and to a lesser extent for guanine transport. A differential response in substrate transport was apparent with PLUTO double mutants E227Q G147Q and E227Q T425A, both of which most strongly affected adenine transport, and in V145A G147Q, which markedly affected guanine transport. These differences could be explained by docking studies, showing that uracil and guanine exhibit a similar binding mode whereas adenine binds deep into the catalytic pocket of PLUTO. Furthermore, competition studies confirmed these results. The present study defines the molecular determinants for PLUTO substrate binding and demonstrates key differences in structure-function relations between PLUTO and other NCS1 family members. PMID:24621654

Structure-function relationship of a plant NCS1 member--homology modeling and mutagenesis identified residues critical for substrate specificity of PLUTO, a nucleobase transporter from Arabidopsis.

PubMed

Witz, Sandra; Panwar, Pankaj; Schober, Markus; Deppe, Johannes; Pasha, Farhan Ahmad; Lemieux, M Joanne; Möhlmann, Torsten

2014-01-01

Plastidic uracil salvage is essential for plant growth and development. So far, PLUTO, the plastidic nucleobase transporter from Arabidopsis thaliana is the only known uracil importer at the inner plastidic membrane which represents the permeability barrier of this organelle. We present the first homology model of PLUTO, the sole plant NCS1 member from Arabidopsis based on the crystal structure of the benzyl hydantoin transporter MHP1 from Microbacterium liquefaciens and validated by molecular dynamics simulations. Polar side chains of residues Glu-227 and backbones of Val-145, Gly-147 and Thr-425 are proposed to form the binding site for the three PLUTO substrates uracil, adenine and guanine. Mutational analysis and competition studies identified Glu-227 as an important residue for uracil and to a lesser extent for guanine transport. A differential response in substrate transport was apparent with PLUTO double mutants E227Q G147Q and E227Q T425A, both of which most strongly affected adenine transport, and in V145A G147Q, which markedly affected guanine transport. These differences could be explained by docking studies, showing that uracil and guanine exhibit a similar binding mode whereas adenine binds deep into the catalytic pocket of PLUTO. Furthermore, competition studies confirmed these results. The present study defines the molecular determinants for PLUTO substrate binding and demonstrates key differences in structure-function relations between PLUTO and other NCS1 family members.

Photochemical aerosol formation in planetary atmospheres: A comparison between Pluto and Titan

NASA Astrophysics Data System (ADS)

Lavvas, Panayotis; Strobel, Darrell F.; Lellouch, Emmanuel; Gurwell, Mark A.; Cheng, Andrew F.; Summers, Michael; Gladstone, Randy

2016-10-01

The New Horizons mission observations have revealed us that Pluto's atmosphere is rich in photochemical hazes that extend to high altitudes above its surface [1], apparently similar to those observed in Titan's atmosphere [2].We use detailed models combining photochemistry and microphysics in order to simulate the aerosol formation and growth in Pluto's atmosphere, as performed for Titan's atmosphere [3]. Here we discuss the possible mechanisms leading to the formation of haze particles in Pluto's atmosphere, and we evaluate the contribution of different growth processes (e.g. coagulation vs. condensation) to the resulting particle properties.Moreover we investigate the role of these particles in the radiative balance of Pluto's atmosphere and we compare the resulting particle properties, with those retrieved for Titan's upper atmosphere based on Cassini observations [4]. We discuss the similarities and difference between Pluto's and Titan's aerosols.[1] Gladstone et al., 2016, Science, 351, 6271[2] West et al., 2015, Titan's Haze, in Titan, Interior, Surface, Atmosphere and Space environment, Cambridge University Press[3] Lavvas et al., 2013, PNAS, pnas.1217059110[4] Lavvas et al., 2015, DPS47, id.205.08

New Horizons Successful Completes the Historic First Flyby of Pluto and Its Moons

NASA Technical Reports Server (NTRS)

Ennico, Kimberly

2015-01-01

On July 14, 2015, after a 9.5 year trek across the solar system, NASA's New Horizons spacecraft flew by the dwarf planet Pluto and its system of moons, taking imagery, spectra and in-situ particle data. Data from New Horizons will address numerous outstanding questions on the geology and composition of Pluto and Charon, plus measurements of Pluto's atmosphere, and provide revised understanding of the formation and evolution of Pluto and Charon and its smaller moons. This data set is an invaluable glimpse into the outer Third Zone of the solar system. Data from the intense July 14th fly-by sequence will be downlinked to Earth over a period of 16 months, the duration set by the large data set (over 60 GBits) and the limited transmitted bandwidth rates (approx. 1-2 kbps) and sharing the three 70 m DSN assets with our missions. The small fraction (approx. 1%) of data downlinked during the early phase of the flyby has already revealed Pluto and Charon to be very different worlds, with increasing and dynamic complexity.

Intrepid: A Mission to Pluto

NASA Technical Reports Server (NTRS)

Behling, Michael; Buchman, Donald; Marcus, Andres; Procopis, Stephanie; Wassgren, Carl; Ziemer, Sarah

1990-01-01

A proposal for an exploratory spacecraft mission to Pluto/Charon system was written in response to the request for proposal for an unmannned probe to pluto (RFP). The design requirements of the RFP are presented and under the guidance of these requirements, the spacecraft Intrepid was designed. The RPF requirement that was of primary importance is the minimization of cost. Also, the reduction of flight time was of extreme importance because the atmosphere of Pluto is expected to collapse close to the Year 2020. If intrepid should arrive after the collapse, the mission would be a failure; for Pluto would be only a solid rock of ice. The topics presented include: (1) scientific instrumentation; (2) mission management, planning, and costing; (3) power and propulsion subsystem; (4) structural subsystem; (5) command, control, and communications; and (6) attitude and articulation control.

A Remarkable World

NASA Image and Video Library

2015-07-03

This image of Pluto and its big moon Charon was taken by NASA's New Horizons spacecraft at 04:15 (UTC) on July 1, 2015, and shows the clearest view yet of the sides of Pluto and Charon that will be studied in great detail during New Horizons' closest approach to the dwarf planet on July 14, 2015. There will be just two more rotations of Pluto and Charon, and two more orbits about their mutual center of gravity, between the time of this image and closest approach (the rotation period of the system is 6.4 days). The image, which has been sharpened by the image processing technique known as deconvolution, shows details as small as about 160 kilometers (100 miles). The highest-resolution images of this side of Pluto, taken on July 14, will show details that are 1,000 times smaller. New Horizons is revealing Pluto to be a world that, at this point, looks like no other in the solar system. Its equatorial regions are occupied by a discontinuous band of very dark material, which is interrupted on this hemisphere by a very bright region which appears sharp-edged at the resolution of the image. The north polar region is blander, but shows a distinctive darker southern boundary where it meets the higher-contrast equatorial regions. The origin of these remarkable features is still unknown, though some of them might be related to seasonal movement of frost across Pluto's surface. Charon, in contrast, still shows few details other than the dark polar region. The image was taken by New Horizons' Long Range Reconnaissance Imager (LORRI ) at a distance from Pluto of 15.8 million kilometers (9.8 million miles) and has a central longitude of 177 degrees on Pluto and 357 degrees on Charon. The inset shows the orientation of Pluto- the solid lines mark the equator and the prime meridian, which is defined to be the longitude that always faces Charon. http://photojournal.jpl.nasa.gov/catalog/PIA19694

Impact and Cratering History of the Pluto System

NASA Astrophysics Data System (ADS)

Greenstreet, Sarah; Gladman, Brett; McKinnon, William B.

2014-11-01

The observational opportunity of the New Horizons spacecraft fly-through of the Pluto system in July 2015 requires a current understanding of the Kuiper belt dynamical sub-populations to accurately interpret the cratering history of the surfaces of Pluto and its satellites. We use an Opik-style collision probability code to compute impact rates and impact velocity distributions onto Pluto and its binary companion Charon from the Canada-France Ecliptic Plane Survey (CFEPS) model of classical and resonant Kuiper belt populations (Petit et al., 2011; Gladman et al., 2012) and the scattering model of Kaib et al. (2011) calibrated to Shankman et al. (2013). Due to the uncertainty in how the well-characterized size distribution for Kuiper belt objects (with diameter d>100 km) connects to smaller objects, we compute cratering rates using three simple impactor size distribution extrapolations (a single power-law, a power-law with a knee, and a power-law with a divot) as well as the "curvy" impactor size distributions from Minton et al. (2012) and Schlichting et al. (2013). Current size distribution uncertainties cause absolute ages computed for Pluto surfaces to be entirely dependent on the extrapolation to small sizes and thus uncertain to a factor of approximately 6. We illustrate the relative importance of each Kuiper belt sub-population to Pluto's cratering rate, both now and integrated into the past, and provide crater retention ages for several cases. We find there is only a small chance a crater with diameter D>200 km has been created on Pluto in the past 4 Gyr. The 2015 New Horizons fly-through coupled with telescope surveys that cover objects with diameters d=10-100 km should eventually drop current crater retention age uncertainties on Pluto to <30%. In addition, we compute the "disruption timescale" (to a factor of three accuracy) for Pluto's smaller satellites: Styx, Nix, Kerberos, and Hydra.

Pluto followed its heart: reorientation and faulting of Pluto due to volatile loading in Sputnik Planum

NASA Astrophysics Data System (ADS)

Tuttle Keane, James; Matsuyama, Isamu; Kamata, Shunichi; Steckloff, Jordan

2016-10-01

The New Horizons flyby of Pluto revealed the dwarf planet to be a strikingly diverse, geologically active world. Perhaps the most intriguing feature on the New Horizons encounter hemisphere is Sputnik Planum—a 1000 km diameter, probable impact basin, filled with several kilometers of actively convecting volatile ices (N2, CH4, CO). One salient characteristic of Sputnik Planum is its curious alignment with the Pluto-Charon tidal axis. The alignment of large geologic features with principal axis of inertia (such as the tidal axis) is the hallmark of global reorientation, i.e. true polar wander. Here we show that the present location of Sputnik Planum is a natural consequence of loading of 1-2 km of volatile ices within the Sputnik Planum basin. Larger volatile ice thicknesses (like those inferred from studies of ice convection within Sputnik Planum) betray an underlying negative gravity anomaly associated with the basin. As Pluto reoriented in response to the loading of volatile ices within Sputnik Planum, stresses accumulated within the lithosphere (as each geographic location experiences a change in tidal/rotational potential). These reorientation stresses, coupled with loading stresses, and stresses from the freezing of a subsurface ocean resulted in the fracturing of Pluto's lithosphere in a characteristic, global pattern of extensional faults. Our predicted pattern of extensional faults due to this reorientation closely replicates the observed distribution of faults on Pluto (more so than global expansion, orbit migration, de-spinning, or loading alone). Sputnik Planum likely formed ~60° northwest of its present location, and was loaded with volatile ices over millions of years due to seasonal volatile transport cycles. This result places Pluto in a truly unique category of planetary bodies where volatiles are not only controlling surface geology and atmospheric processes, but they are also directly controlling the orientation of the entire dwarf planet. Pluto's past, present, and future orientation is controlled by complicated feedbacks between volatile transport, insolation, and interior structure.

The Cold and Icy Heart of Pluto

NASA Astrophysics Data System (ADS)

Hamilton, D. P.

2015-12-01

The locations of large deposits of frozen volatiles on planetary surfaces are largely coincident with areas receiving the minimum annual influx of solar energy. Thus we have the familiar polar caps of Earth and Mars, but cold equatorial regions for planets with obliquities between 54 and 126 degrees. Furthermore, for tilts between 45-66 degrees and 114-135 degrees the minimum incident energy occurs neither at the pole nor the equator. We find that the annual average insolation is always symmetric about Pluto's equator and is fully independent of the relative locations of the planet's pericenter and equinoxes. Remarkably, this symmetry holds for arbitrary orbital eccentricities and obliquities, and so we provide a short proof in the margin of this abstract. The current obliquity of Pluto is 119 degrees, giving it minima in average annual insolation at +/- 27 degrees latitude, with ~1.5% more flux to the equator and ~15% more to the poles. But the obliquity of Pluto also varies sinusoidally from 102-126 degrees and so, over the past million years, Pluto's annual equatorial and polar fluxes have changed by +15% and -13%, respectively. Interestingly, the energy flux received by latitudes between 25-35 degrees remains nearly constant over the presumably billions of years since Pluto acquired its current orbit and spin properties. Thus these latitudes are continuously cold and should be favored for the long-term deposition of volatile ices; the bright heart of Pluto, Sputnik Planum, extends not coincidentally across these latitudes. Reflected light and emitted thermal radiation from Charon increases annual insolation to one side of Pluto by of order 0.02%. Although small, the bulk of the energy is delivered at night to Pluto's cold equatorial regions. Furthermore, Charon's thermal IR is delivered very efficiently to icy deposits. Over billions of years, ices have preferentially formed and survived in the anti-Charon hemisphere.

The Extraordinary Albedo Variations on Pluto Detected by New Horizons and Implications for Dwarf Planet Eris

NASA Astrophysics Data System (ADS)

Buratti, Bonnie J.; Hofgartner, Jason D.; Stern, S. Alan; Weaver, Harold A.; Verbiscer, Anne J.; Ennico, Kimberly; Olkin, Catherine B.; Young, Leslie; New Horizons Geology and Geophysics Team

2016-10-01

The New Horizons mission returned stunning observations of active geology on the surface of Pluto (Stern et al., 2015, Science 350, 292). One of the markers for activity on planets or moons is normal albedos approaching 1.0, as is the case for Enceladus (Buratti et al., 1984, Icarus 58, 254; Verbiscer et al., 2005, Icarus 173, 66). When all corrections for viewing geometry are made for Pluto, it has normal albedos that approach unity in the regions that show evidence for activity by a lack of craters, notably the region informally named Sputnik Planum. On the other hand, Pluto also has a very dark (normal albedo ~0.10) equatorial belt.The geometric albedo of Eris, another large dwarf planet in the Kuiper Belt, is 0.96 (Sicardy et al., 2011, Nature 478, 493), close to that of Enceladus. Coupled with a high density of 2.5 gm/cc (Sicardy et al., ibid.), implying an even larger amount of radiogenic heating than that for Pluto (with a density near 1.9 gm/cc), we find it highly likely that Eris is also active with some type of solid state convection or cryovolcanism on its surface. Alternate explanations such as complete condensation of methane frost onto its surface in the colder environment at nearly 100 AUs would not lead to the high albedo observed.Another implication of the extreme albedo variations on Pluto is that the temperature varies by at least 20K on its surface, spawning possible aeolian processes and associated features such as wind streaks and dunes, which are currently being sought on New Horizons images. Finally, low albedo regions on Pluto, with normal reflectances less than 0.10, provide possible evidence for dust in the Kuiper Belt that is accreting onto the surface of Pluto. Another - or additional - explanation for this low-albedo dust is native material created in Pluto's hazy atmosphere.New Horizons funding by NASA is gratefully acknowledged.

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

Dr. Alan Stern, New Horizons principal investigator, speaks on a panel at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. Scientists discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

Dr. Jim Green, Dr. Ed Stone, and Dr. Alan Stern speak on a panel at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. They discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

Dr. Ed Stone, Voyager project scientist, speaks on a panel at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. Scientists discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

Dr. Jim Green, Director of NASA’s Planetary Division, speaks on a panel at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. Scientists discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

The impactor flux in the Pluto-Charon system

NASA Technical Reports Server (NTRS)

Weissman, Paul R.; Stern, S. Alan

1994-01-01

Current impact rates of comets on Pluto and Charon are estimated. It is shown that the dominant sources of impactors are comets from the Kuiper belt and the inner Oort cloud, each of whose perihelion distribution extends across Pluto's orbit. In contrast, long-period comets from the outer Oort cloud are a negligible source of impactors. The total predicted number of craters is not sufficient to saturate the surface areas of either Pluto of Charon over the age of the Solar System. However, heavy cratering may have occurred early in the Solar System's history during clearing of planetesimals from the outer planets' zone.

Ice Volcanoes on Pluto?

NASA Image and Video Library

2015-11-10

NASA New Horizons scientists believe that the informally named feature Wright Mons, located south of Sputnik Planum on Pluto, and another, Piccard Mons, could have been formed by the cryovolcanic eruption of ices from beneath Pluto surface. Sputnik Planum on Pluto, is an unusual feature that's about 100 miles (160 kilometers) wide and 13,000 feet (4 kilometers) high. It displays a summit depression (visible in the center of the image) that's approximately 35 miles (56 kilometers) across, with a distinctive hummocky texture on its sides. The rim of the summit depression also shows concentric fracturing. http://photojournal.jpl.nasa.gov/catalog/PIA20155

CVF spectrophotometry of Pluto - Correlation of composition with albedo. [circularly variable filter

NASA Technical Reports Server (NTRS)

Marcialis, Robert L.; Lebofsky, Larry A.

1991-01-01

The present time-resolved, 0.96-2.65-micron spectrophotometry for the Pluto-Charon system indicates night-to-night variations in the depths of the methane absorptions such that the bands' equivalent width is near minimum light. The interpretation of these data in terms of a depletion of methane in dark regions of the planet, relative to bright ones, is consistent with the Buie and Fink (1987) observations. The near-IR spectrum of Pluto seems to be dominated by surface frost. It is suggested that the dark equatorial regions of Pluto are redder than those of moderate albedo.

Spectrophotometry of Pluto-Charon mutual events - Individual spectra of Pluto and Charon

NASA Technical Reports Server (NTRS)

Sawyer, S. R.; Barker, E. S.; Cochran, A. L.; Cochran, W. D.

1987-01-01

Time-resolved spectra of the March 3 and April 4, 1987 mutual events of Pluto and Charon, obtained with spectral coverage from 5500 to 10,000 A with 25-A spectral resolution, are discussed. Charon has a featureless reflectance spectrum, with no evidence of methane absorption. Charon's reflectance appears neutral in color and corresponds to a geometric albedo of about 0.37 at 6000 A. The Pluto reflectance spectrum displays methane absorption bands at 7300, 7900, 8400, 8600, and 8900 A and is red in color, with a geometric albedo of about 0.56 at 6000 A.

Flight set 360T004 (STS-30)

NASA Technical Reports Server (NTRS)

Nelsen, Lowell V.

1990-01-01

The performance of 360T004, Forth Flight, Redesigned Solid Rocket Motors (RSRM) is assessed in respect to joint sealing issues as seen from post-test inspection of the seals and sealing surfaces. The factory joint disassembly inspections for this flight set were omitted. The decision was based on the rational that there is sufficient information in the present data base, and this would give H-7 refurbishment operations faster turn around time for this set of hardware. The factory joint disassembly inspections will resume for 360H005, Fifth Flight, through 360L007, Seventh Flight, due to a new grease application being in effect during the assembly process. The left hand nozzle was forced into the snubbed position upon splash down. This required unique tooling to be manufactured to perform the disassembly of the internal nozzle joints. This was completed on February 5 and 6, 1990 at the H-5 Clearfield, Utah facility. The RSRM consisting of capture feature, field joints with the J-joint insulation configuration is illustrated. The nozzle-to-case joint design, which includes 100, 7/8-inch radial bolts in conjunction with a wiper O-ring and modified insulation design is also illustrated, as is the ignition system seals and a cross section of the igniter. The configuration of all internal nozzle joints is shown.

Postflight hardware evaluation 360T026 (RSRM-26, STS-47)

NASA Technical Reports Server (NTRS)

Nielson, Greg

1993-01-01

The final report for the Clearfield disassembly evaluation and a continuation of the KSC postflight assessment for the 360T026 (STS-47) Redesigned Solid Rocket Motor (RSRM) flight set is provided. All observed hardware conditions were documented on PFOR's and are included in Appendices A, B, and C. Appendices D and E contain the measurements and safety factor data for the nozzle and insulation components. This report, along with the KSC Ten-Day Postflight Hardware Evaluation Report (TWR-64203), represents a summary of the 360T026 hardware evaluation. The as-flown hardware configuration is documented in TWR-60472. Disassembly evaluation photograph numbers are logged in TWA-1987. The 360T026 flight set disassembly evaluations described were performed at the RSRM Refurbishment Facility in Clearfield, Utah. The final factory joint demate occurred on 12 April 1993. Detailed evaluations were performed in accordance with the Clearfield Postflight Engineering Evaluation Plan (PEEP), TWR-50051, Revision A. All observations were compared against limits that are also defined in the PEEP. These limits outline the criteria for categorizing the observations as acceptable, reportable, or critical. Hardware conditions that were unexpected and/or determined to be reportable or critical were evaluated by the applicable CPT and tracked through the PFAR system.

Problems Encountered During the Recertification of the GLORY Solar Array Dual Axis Gimbal Drive Actuators

NASA Technical Reports Server (NTRS)

Saltzman, Marc; Schepis, Jospeh P.; Bruckner, Michael J.

2009-01-01

The Glory observatory is the current incarnation of the Vegetation Canopy Lidar (VCL) mission spacecraft bus. The VCL spacecraft bus, having been cancelled for programmatic reasons in 2000, was nearly integrated when it was put into storage for possible future use. The Glory mission was a suitable candidate for using this spacecraft and in 2006 an effort to recertify the two axis solar array gimbal drive after its extended storage was begun. What was expected to be a simple performance validation of the two dual axis gimbal stepper motors became a serious test, diagnosis and repair task once questions arose on the flight worthiness of the hardware. A significant test program logic flow was developed which identified decisions that could be made based on the results of individual recertification tests. Without disassembling the bi-axial gimbals, beginning with stepper motor threshold voltage measurements and relating these to powered drive torque measurements, both performed at the spacecraft integrator s facility, a confusing picture of the health of the actuators came to light. Tests at the gimbal assembly level and tests of the disassembled actuators were performed by the manufacturer to validate our results and torque discrepancies were noted. Further disassembly to the component level of the actuator revealed the source of the torque loss.

The trans-neptunian object UB313 is larger than Pluto.

PubMed

Bertoldi, F; Altenhoff, W; Weiss, A; Menten, K M; Thum, C

2006-02-02

The most distant known object in the Solar System, 2003 UB313 (97 au from the Sun), was recently discovered near its aphelion. Its high eccentricity and inclination to the ecliptic plane, along with its perihelion near the orbit of Neptune, identify it as a member of the 'scattered disk'. This disk of bodies probably originates in the Kuiper belt objects, which orbit near the ecliptic plane in circular orbits between 30 and 50 au, and may include Pluto as a member. The optical brightness of 2003 UB313, if adjusted to Pluto's distance, is greater than that of Pluto, which suggested that it might be larger than Pluto. The actual size, however, could not be determined from the optical measurements because the surface reflectivity (albedo) was unknown. Here we report observations of the thermal emission of 2003 UB313 at a wavelength of 1.2 mm, which in combination with the measured optical brightness leads to a diameter of 3,000 +/- 300 +/- 100 km. Here the first error reflects measurement uncertainties, while the second derives from the unknown object orientation. This makes 2003 UB313 the largest known trans-neptunian object, even larger than Pluto (2,300 km). The albedo is 0.60 +/- 0.10 +/- 0.05, which is strikingly similar to that of Pluto, suggesting that the methane seen in the optical spectrum causes a highly reflective icy surface.

Pluto at High Noon Artist Concept

NASA Image and Video Library

2015-06-08

Just how dim is the sunlight on Pluto, some three billion miles away? This artist concept of the frosty surface of Pluto with Charon and our sun as backdrops illustrates that while sunlight is much weaker than it is here on Earth, it isnt as dark as you might expect. http://photojournal.jpl.nasa.gov/catalog/PIA19682

PLUTO AND CHARON WITH THE HUBBLE SPACE TELESCOPE. I. MONITORING GLOBAL CHANGE AND IMPROVED SURFACE PROPERTIES FROM LIGHT CURVES

DOE Office of Scientific and Technical Information (OSTI.GOV)

Buie, Marc W.; Young, Eliot F.; Young, Leslie A.

We present new light-curve measurements of Pluto and Charon taken with the Advanced Camera for Surveys High-resolution Camera on the Hubble Space Telescope. The observations were collected from 2002 June to 2003 June at 12 distinct sub-Earth longitudes over a range of solar phase angle 0.{sup 0}36-1.{sup 0}74-a larger range than previously measured. The new measurements of Pluto show that the light-curve amplitude has decreased since the mutual event season in the late 1980s. We also show that the average brightness has increased in the F555W (Johnson V equivalent) passband while the brightness has decreased in the F435W (Johnson Bmore » equivalent) passband. These data thus indicate a substantial reddening of the reflected light from Pluto. We find a weighted mean (B - V) = 0.9540 {+-} 0.0010 that is considerably higher than the long-standing value of (B - V) = 0.868 {+-} 0.003 most recently measured in 1992-1993. This change in color cannot be explained by the evolving viewing geometry and provides the strongest evidence to date for temporal changes on the surface of Pluto that are expected to be linked to volatile transport processes. We also report on the discovery of a new rotational modulation of Pluto's hemispherical color that ranges from 0.92 to 0.98 with the least red color at the longitude of maximum light and most red at minimum light. The phase coefficient of Pluto is nearly the same as measured in 1992-1993 with a value of {beta} {sub B} = 0.0392 {+-} 0.0064 and {beta} {sub V} = 0.0355 {+-} 0.0045 mag deg{sup -1} for the F435W and F555W data, respectively. The Pluto phase curve is still very close to linear but a small but significant nonlinearity is seen in the data. In contrast, the light curve of Charon is essentially the same as in 1992/1993, albeit with much less noise. We confirm that Charon's Pluto-facing hemisphere is 8% brighter than the hemisphere facing away from Pluto. The color of Charon is independent of longitude and has a mean weighted value of (B - V) = 0.7315 {+-} 0.0013. The phase curve for Charon is now shown to be strongly nonlinear and wavelength dependent. We present results for both Pluto and Charon that better constrain the single-particle scattering parameters from the Hapke scattering theory.« less

Pluto's Volatile Transport

NASA Astrophysics Data System (ADS)

Young, Leslie

2012-10-01

Pluto's varying subsolar latitude and heliocentric distance leads to large variations in the surface volatile distribution and surface pressure. I present results of new volatile transport models (Young 2012a, b). The models include insolation, thermal emission, subsurface conduction, heating of a volatile slab, internal heat flux, latent heat of sublimation, and strict global mass balance. Numeric advances include initial conditions that allow for rapid convergence, efficient computation with matrix arithmetic, and stable Crank-Nicholson timesteps for both bare and volatile-covered areas. Runs of the model show six distinct seasons on Pluto. (1) As Pluto approaches perihelion, the volatiles on the old winter pole (the Rotational North Pole, RNP) becomes more directly illuminated , and the pressure and albedo rise rapidly. (2) When a new ice cap forms on the Rotational South Pole, RSP, volatiles are exchanged between poles. The pressure and albedo change more slowly. (3) When all volatiles have sublimed from the RNP, the albedo and pressure drop rapidly. (4-6) A similar pattern is repeated near aphelion with a reversal of the roles and the poles. I will compare results with earlier Pluto models of Hansen and Paige (1996), show the dependence on parameters such as substrate inertia, and make predictions for the New Horizons flyby of Pluto in 2015. This work was supported, in part, by funding from NASA Planetary Atmospheres Grant NNG06GF32G and the Spitzer project (JPL research support Agreement 1368573). Hansen, C. J. and D. A. Paige 1996. Seasonal Nitrogen Cycles on Pluto. Icarus 120, 247-265. Young, L. A. 2012a. Volatile transport on inhomogeneous surfaces: I - Analytic expressions, with application to Pluto’s day. Icarus, in press Young, L. A. 2012b. Volatile transport on inhomogeneous surfaces: II. Numerical calculations, with application to Pluto's season. In preparation.

PLUTO AND CHARON WITH THE HUBBLE SPACE TELESCOPE. II. RESOLVING CHANGES ON PLUTO'S SURFACE AND A MAP FOR CHARON

DOE Office of Scientific and Technical Information (OSTI.GOV)

Buie, Marc W.; Young, Eliot F.; Young, Leslie A.

We present new imaging of the surface of Pluto and Charon obtained during 2002-2003 with the Hubble Space Telescope (HST) Advanced Camera for Surveys (ACS) instrument. Using these data, we construct two-color albedo maps for the surfaces of both Pluto and Charon. Similar mapping techniques are used to re-process HST/Faint Object Camera (FOC) images taken in 1994. The FOC data provide information in the ultraviolet and blue wavelengths that show a marked trend of UV-bright material toward the sunlit pole. The ACS data are taken at two optical wavelengths and show widespread albedo and color variegation on the surface ofmore » Pluto and hint at a latitudinal albedo trend on Charon. The ACS data also provide evidence for a decreasing albedo for Pluto at blue (435 nm) wavelengths, while the green (555 nm) data are consistent with a static surface over the one-year period of data collection. We use the two maps to synthesize a true visual color map of Pluto's surface and investigate trends in color. The mid- to high-latitude region on the sunlit pole is, on average, more neutral in color and generally higher albedo than the rest of the surface. Brighter surfaces also tend to be more neutral in color and show minimal color variations. The darker regions show considerable color diversity arguing that there must be a range of compositional units in the dark regions. Color variations are weak when sorted by longitude. These data are also used to constrain astrometric corrections that enable more accurate orbit fitting, both for the heliocentric orbit of the barycenter and the orbit of Pluto and Charon about their barycenter.« less

Pluto's Atmosphere, Then and Now

NASA Astrophysics Data System (ADS)

Elliot, J. L.; Buie, M.; Person, M. J.; Qu, S.

2002-09-01

The KAO light curve for the 1988 stellar occultation by Pluto exhibits a sharp drop just below half light, but above this level the light curve is consistent with that of an isothermal atmosphere (T = 105 +/- 8 K, with N2 as its major constituent). The sharp drop in the light curve has been interpreted as being caused by: (i) a haze layer, (ii) a large thermal gradient, or (iii) some combination of these two. Modeling Pluto's atmosphere with a haze layer yields a normal optical depth >= 0.145 (Elliot & Young 1992, AJ 103, 991). On the other hand, if Pluto's atmosphere is assumed to be clear, the occultation light curve can be inverted with a new method that avoids the large-body approximations. Inversion of the KAO light curve with this method yields an upper isothermal part, followed by a sharp thermal gradient that reaches a maximum magnitude of -3.9 +/- 0.6 K km-1 at the end of the inversion (r = 1206 +/- 10 km). Even though we do not yet understand the cause of the sharp drop, the KAO light curve can be used as a benchmark for examining subsequent Pluto occultation light curves to determine whether Pluto's atmospheric structure has changed since 1988. As an example, the Mamiña light curve for the 2002 July 20 Pluto occultation of P126A was compared with the KAO light curve by Buie et al. (this conference), who concluded that Pluto's atmospheric structure has changed significantly since 1988. Further analysis and additional light curves from this and subsequent occultations (e.g. 2002 August 21) will allow us to elucidate the nature of these changes. This work was supported, in part, by grants from NASA (NAG5-9008 and NAG5-10444) and NSF (AST-0073447).

The Orbits and Masses of Pluto's Satellites

NASA Astrophysics Data System (ADS)

Brozovic, Marina; Jacobson, R. A.

2013-05-01

Abstract (2,250 Maximum Characters): We report on the numerically integrated orbital fits of Pluto's satellites, Charon, Nix, Hydra, and S/2011 (134340) 1, to an extensive set of astrometric, mutual event, and stellar occultation observations over the time interval April 1965 to July 2011. The observations of Charon relative to Pluto have been corrected for the Pluto center-of-figure center-of-light (COF) offset due to the Pluto albedo variations. The most recently discovered satellite S/2012 (134340) 1 is fit with a precessing ellipse because its observation set is insufficient to constrain a numerically integrated orbit. The Pluto system mass is well determined with the current data. However, the Charon’s mass still carries a considerable amount of the uncertainty due to the fact that the primary source of information for the Charon mass is a small quantity of absolute position measurements that are sensitive to the independent motions of Pluto and Charon about the system barycenter. We used bounded-least squares algorithm to try to constrain the masses of Nix, Hydra, and S/2011 (134340) 1, but the current dataset appears to be too sparse for mass determination. The long-term dynamical interaction among the satellites does yield a weak determination of Hydra's mass. We investigated the effect of more astrometry of S/2012 (134340) 1 on the mass determination of the other satellites and found no improvement with the additional data. We have delivered ephemerides based on our integrated orbits to the New Horizons project along with their expected uncertainties at the time of the spacecraft encounter with the Pluto system. Acknowledgments: The research described in this paper was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

The atmosphere of Pluto as observed by New Horizons

NASA Astrophysics Data System (ADS)

Gladstone, G. Randall; Stern, S. Alan; Ennico, Kimberly; Olkin, Catherine B.; Weaver, Harold A.; Young, Leslie A.; Summers, Michael E.; Strobel, Darrell F.; Hinson, David P.; Kammer, Joshua A.; Parker, Alex H.; Steffl, Andrew J.; Linscott, Ivan R.; Parker, Joel Wm.; Cheng, Andrew F.; Slater, David C.; Versteeg, Maarten H.; Greathouse, Thomas K.; Retherford, Kurt D.; Throop, Henry; Cunningham, Nathaniel J.; Woods, William W.; Singer, Kelsi N.; Tsang, Constantine C. C.; Schindhelm, Eric; Lisse, Carey M.; Wong, Michael L.; Yung, Yuk L.; Zhu, Xun; Curdt, Werner; Lavvas, Panayotis; Young, Eliot F.; Tyler, G. Leonard; Bagenal, F.; Grundy, W. M.; McKinnon, W. B.; Moore, J. M.; Spencer, J. R.; Andert, T.; Andrews, J.; Banks, M.; Bauer, B.; Bauman, J.; Barnouin, O. S.; Bedini, P.; Beisser, K.; Beyer, R. A.; Bhaskaran, S.; Binzel, R. P.; Birath, E.; Bird, M.; Bogan, D. J.; Bowman, A.; Bray, V. J.; Brozovic, M.; Bryan, C.; Buckley, M. R.; Buie, M. W.; Buratti, B. J.; Bushman, S. S.; Calloway, A.; Carcich, B.; Conard, S.; Conrad, C. A.; Cook, J. C.; Cruikshank, D. P.; Custodio, O. S.; Ore, C. M. Dalle; Deboy, C.; Dischner, Z. J. B.; Dumont, P.; Earle, A. M.; Elliott, H. A.; Ercol, J.; Ernst, C. M.; Finley, T.; Flanigan, S. H.; Fountain, G.; Freeze, M. J.; Green, J. L.; Guo, Y.; Hahn, M.; Hamilton, D. P.; Hamilton, S. A.; Hanley, J.; Harch, A.; Hart, H. M.; Hersman, C. B.; Hill, A.; Hill, M. E.; Holdridge, M. E.; Horanyi, M.; Howard, A. D.; Howett, C. J. A.; Jackman, C.; Jacobson, R. A.; Jennings, D. E.; Kang, H. K.; Kaufmann, D. E.; Kollmann, P.; Krimigis, S. M.; Kusnierkiewicz, D.; Lauer, T. R.; Lee, J. E.; Lindstrom, K. L.; Lunsford, A. W.; Mallder, V. A.; Martin, N.; McComas, D. J.; McNutt, R. L.; Mehoke, D.; Mehoke, T.; Melin, E. D.; Mutchler, M.; Nelson, D.; Nimmo, F.; Nunez, J. I.; Ocampo, A.; Owen, W. M.; Paetzold, M.; Page, B.; Pelletier, F.; Peterson, J.; Pinkine, N.; Piquette, M.; Porter, S. B.; Protopapa, S.; Redfern, J.; Reitsema, H. J.; Reuter, D. C.; Roberts, J. H.; Robbins, S. J.; Rogers, G.; Rose, D.; Runyon, K.; Ryschkewitsch, M. G.; Schenk, P.; Sepan, B.; Showalter, M. R.; Soluri, M.; Stanbridge, D.; Stryk, T.; Szalay, J. R.; Tapley, M.; Taylor, A.; Taylor, H.; Umurhan, O. M.; Verbiscer, A. J.; Versteeg, M. H.; Vincent, M.; Webbert, R.; Weidner, S.; Weigle, G. E.; White, O. L.; Whittenburg, K.; Williams, B. G.; Williams, K.; Williams, S.; Zangari, A. M.; Zirnstein, E.

2016-03-01

Observations made during the New Horizons flyby provide a detailed snapshot of the current state of Pluto's atmosphere. Whereas the lower atmosphere (at altitudes of less than 200 kilometers) is consistent with ground-based stellar occultations, the upper atmosphere is much colder and more compact than indicated by pre-encounter models. Molecular nitrogen (N2) dominates the atmosphere (at altitudes of less than 1800 kilometers or so), whereas methane (CH4), acetylene (C2H2), ethylene (C2H4), and ethane (C2H6) are abundant minor species and likely feed the production of an extensive haze that encompasses Pluto. The cold upper atmosphere shuts off the anticipated enhanced-Jeans, hydrodynamic-like escape of Pluto's atmosphere to space. It is unclear whether the current state of Pluto's atmosphere is representative of its average state - over seasonal or geologic time scales.

The atmosphere of Pluto as observed by New Horizons.

PubMed

Gladstone, G Randall; Stern, S Alan; Ennico, Kimberly; Olkin, Catherine B; Weaver, Harold A; Young, Leslie A; Summers, Michael E; Strobel, Darrell F; Hinson, David P; Kammer, Joshua A; Parker, Alex H; Steffl, Andrew J; Linscott, Ivan R; Parker, Joel Wm; Cheng, Andrew F; Slater, David C; Versteeg, Maarten H; Greathouse, Thomas K; Retherford, Kurt D; Throop, Henry; Cunningham, Nathaniel J; Woods, William W; Singer, Kelsi N; Tsang, Constantine C C; Schindhelm, Eric; Lisse, Carey M; Wong, Michael L; Yung, Yuk L; Zhu, Xun; Curdt, Werner; Lavvas, Panayotis; Young, Eliot F; Tyler, G Leonard

2016-03-18

Observations made during the New Horizons flyby provide a detailed snapshot of the current state of Pluto's atmosphere. Whereas the lower atmosphere (at altitudes of less than 200 kilometers) is consistent with ground-based stellar occultations, the upper atmosphere is much colder and more compact than indicated by pre-encounter models. Molecular nitrogen (N2) dominates the atmosphere (at altitudes of less than 1800 kilometers or so), whereas methane (CH4), acetylene (C2H2), ethylene (C2H4), and ethane (C2H6) are abundant minor species and likely feed the production of an extensive haze that encompasses Pluto. The cold upper atmosphere shuts off the anticipated enhanced-Jeans, hydrodynamic-like escape of Pluto's atmosphere to space. It is unclear whether the current state of Pluto's atmosphere is representative of its average state--over seasonal or geologic time scales. Copyright © 2016, American Association for the Advancement of Science.

Pluto Majestic Mountains, Frozen Plains and Foggy Hazes

NASA Image and Video Library

2015-09-17

Just 15 minutes after its closest approach to Pluto on July 14, 2015, NASA's New Horizons spacecraft looked back toward the sun and captured this near-sunset view of the rugged, icy mountains and flat ice plains extending to Pluto's horizon. The smooth expanse of the informally named icy plain Sputnik Planum (right) is flanked to the west (left) by rugged mountains up to 11,000 feet (3,500 meters) high, including the informally named Norgay Montes in the foreground and Hillary Montes on the skyline. To the right, east of Sputnik, rougher terrain is cut by apparent glaciers. The backlighting highlights more than a dozen layers of haze in Pluto's tenuous but distended atmosphere. The image was taken from a distance of 11,000 miles (18,000 kilometers) to Pluto; the scene is 780 miles (1,250 kilometers) wide. http://photojournal.jpl.nasa.gov/catalog/PIA19948

The Geology of Pluto and Charon Through the Eyes of New Horizons

NASA Technical Reports Server (NTRS)

Moore, J. M.; McKinnon, W. B.; Spencer, J. R.; Howard, A. D.; Schenk, P. M.; Beyer, R. A.; Nimmo, F.; Singer, K. N.; Umurhan, O. M.; White, O. L.;

Pluto Express - Out of the Darkness

NASA Technical Reports Server (NTRS)

Herman, M.

1995-01-01

Pluto, discovered in 1930, is the largest of a class of primordial bodies at the edge of our solar system that have comet-like properties and remain relatively unmodified by warming from the sun. It is the only planet in the solar system not explored via robotic spacecraft. This lecture discusses the status of the Pluto Express preproject (science objectives, etc.), and its telecommunication subsystem.

New Horizons Event: The First Mission to the Pluto System

NASA Image and Video Library

2014-08-25

Audience members view slides from a presentation by Dr. Jim Green, Dr. Ed Stone, and Dr. Alan Stern at the "New Horizons: The First Mission to the Pluto System and the Kuiper Belt" Event at NASA Headquarters in Washington, DC Monday, August 25, 2014. They discussed how the first images of Pluto and its moons would be captured by the New Horizons spacecraft during a five month long reconnaissance flyby study starting in the summer of 2015. New Horizons launched on January 19, 2006 and is scheduled to make its closest approach to Pluto on July 14, 2015. Photo Credit: (NASA/Aubrey Gemignani)

Kuiper Belt Objects Along the Pluto-Express Path

NASA Technical Reports Server (NTRS)

Jewitt, David (Principal Investigator)

1997-01-01

The science objective of this work is to identify objects in the Kuiper Belt which will, in the 5 years following Pluto encounter, be close to the flight path of NASA's Pluto Express. Our hope is that we will find a Kuiper Belt object or objects close enough that a spacecraft flyby will be possible. If we find a suitable object, the science yield of Pluto Express will be substantially enhanced. The density of objects in the Kuiper Belt is such that we are reasonably likely to find an object close enough to the flight path that on-board gas thrusters can effect a close encounter.

Charon/Pluto Mass Ratio Obtained with HST CCD Observations in 1991 and 1993

NASA Technical Reports Server (NTRS)

Null, George W.

1995-01-01

We have analyzed Hubble Space Telescope wide field camera observations of Pluto, Charon, and a reference star, acquired in 1991 and 1993, to observe Pluto's barycentric motion and determine the Charon/Pluto mass ratio, q = 0.1237 +/-0.0081, with 6.5% accuracy. Solution values for Charon orbital elements include the semimajor axis, a = 19662 +/-81 km; inclination, i = 96.57 +/-0.24 deg; eccentricity, e = 0.0072 +/-0.0067; longitude of periapsis, w = 2 +/-35 deg; and mean longitude, l = 123.58 +/-0.43 deg. These elements are referred to the J2000 Earth equator and equinox at epoch JED 2446600.5.

Looking over Pluto

NASA Image and Video Library

2015-09-10

This synthetic perspective view of Pluto, based on the latest high-resolution images to be downlinked from NASA's New Horizons spacecraft, shows what you would see if you were approximately 1,100 miles (1,800 kilometers) above Pluto's equatorial area, looking northeast over the dark, cratered, informally named Cthulhu Regio toward the bright, smooth, expanse of icy plains informally called Sputnik Planum. The entire expanse of terrain seen in this image is 1,100 miles (1,800 kilometers) across. The images were taken as New Horizons flew past Pluto on July 14, 2015, from a distance of 50,000 miles (80,000 kilometers). http://photojournal.jpl.nasa.gov/catalog/PIA19937

The Other Red Planet Animation

NASA Image and Video Library

2015-07-03

What color is Pluto? The answer, revealed in the first maps made from New Horizons data, turns out to be shades of reddish brown. The mission's first map of Pluto is in approximate true color -- that is, the color you would see if you were riding on New Horizons. At left, a map of Pluto's northern hemisphere composed using high-resolution black-and-white images from New Horizons LORRI instrument. At right is a map of Pluto's colors created using data from the Ralph instrument. In the center is the combined map, produced by merging the LORRI and Ralph data. http://photojournal.jpl.nasa.gov/catalog/PIA19697

The formation of Charon's red poles from seasonally cold-trapped volatiles

NASA Astrophysics Data System (ADS)

Grundy, W. M.; Cruikshank, D. P.; Gladstone, G. R.; Howett, C. J. A.; Lauer, T. R.; Spencer, J. R.; Summers, M. E.; Buie, M. W.; Earle, A. M.; Ennico, K.; Parker, J. Wm.; Porter, S. B.; Singer, K. N.; Stern, S. A.; Verbiscer, A. J.; Beyer, R. A.; Binzel, R. P.; Buratti, B. J.; Cook, J. C.; Dalle Ore, C. M.; Olin, C. B.; Parker, A. H.; Protopapa, S.; Quirico, E.; Retherford, K. D.; Robbins, S. J.; Schmitt, B.; Stansberry, J. A.; Umurhan, O. M.; Weaver, H. A.; Young, L. A.; Zangari, A. M.; Bray, V. J.; Cheng, A. F.; McKinnon, W. B.; McNutt, R. L.; Morre, J. M.; Nimmo, F.; Reuter, D. C.; Schenk, P. M.; New Horizons Science Team; Stern, S. A.; Bagenal, F.; Ennico, K.; Gladstone, G. R.; Grundy, W. M.; McKinnon, W. B.; Moore, J. M.; Olkin, C. B.; Spencer, J. R.; Weaver, H. A.; Young, L. A.; Andert, T.; Barnouin, O.; Beyer, R. A.; Binzel, R. P.; Bird, M.; Bray, V. J.; Brozovic, M.; Buie, M. W.; Buratti, B. J.; Cheng, A. F.; Cook, J. C.; Cruikshank, D. P.; Dalle Ore, C. M.; Earler, A. M.; Elliott, H. A.; Greathouse, T. K.; Hahn, M.; Hamilton, D. P.; Hill, M. E.; Hinson, D. P.; Hofgartner, J.; Horányi, M.; Howard, A. D.; Howett, C. J. A.; Jennings, D. E.; Kammer, J. A.; Kollmann, P.; Lauer, T. R.; Lavvas, P.; Linscott, I. R. Lisse, C. M.; Lunsford, A. W.; McComas, D. J.; McNutt, R. L., Jr.; Mutchler, M.; Nimmo, F.; Nunez, J. I.; Paetzold, M.; Parker, A. H.; Parker, J. Wm.; Philippe, S.; Piquette, M.; Porter, S. B.; Protopapa, S.; Quirico, E.; Reitsema, H. J.; Reuter, D. C.; Robbins, S. J.; Roberts, J. H.; Runyon, K.; Schenk, P. M.; Schindhelm, E.; Schmitt, B.; Showalter, M. R.; Singer, K. N.; Stansberry, J. A.; Steffl, A. J.; Strobel, D. F.; Stryk, T.; Summers, M. E.; Szalay, J. R.; Throop, H. B.; Tsang, C. C. C.; Tyler, G. L.; Umurhan, O. M.; Verbiscer, A. J.; Versteeg, M. H.; Weigle, G. E., II; White, O. L.; Woods, W. W.; Young, E. F.; Zangari, A. M.

2016-11-01

A unique feature of Pluto's large satellite Charon is its dark red northern polar cap. Similar colours on Pluto's surface have been attributed to tholin-like organic macromolecules produced by energetic radiation processing of hydrocarbons. The polar location on Charon implicates the temperature extremes that result from Charon's high obliquity and long seasons in the production of this material. The escape of Pluto's atmosphere provides a potential feedstock for a complex chemistry. Gas from Pluto that is transiently cold-trapped and processed at Charon's winter pole was proposed as an explanation for the dark coloration on the basis of an image of Charon's northern hemisphere, but not modelled quantitatively. Here we report images of the southern hemisphere illuminated by Pluto-shine and also images taken during the approach phase that show the northern polar cap over a range of longitudes. We model the surface thermal environment on Charon and the supply and temporary cold-trapping of material escaping from Pluto, as well as the photolytic processing of this material into more complex and less volatile molecules while cold-trapped. The model results are consistent with the proposed mechanism for producing the observed colour pattern on Charon.

The New Horizons Bistatic Radio Science Experiment to Measure Pluto's Surface Properties

NASA Astrophysics Data System (ADS)

Linscott, I.; Hinson, D. P.; Tyler, G. L.; Vincent, M.

2014-12-01

The New Horizons (NH) payload includes a Radio Science Experiment (REX) for principally occultation and radiometric measurement of Pluto and Charon during the flyby in July 2015. The REX subsystem is contained, together with the NH X-Band radio, in the Integrated Electronics Module (IEM) in the New Horizons spacecraft. REX samples and records in two polarizations both total RF power in a 4.5 MHz bandwidth, and radio signal waveforms in a narrow, 1.25 kHz band. During the encounter, and at closest approach to Pluto, the spacecraft's high gain antenna (HGA) will scan Pluto's equatorial latitudes, intercepting the specular zone, a region near Pluto's limb that geometrically favors reflection from the earth's direction. At the same time, a powerful 80 kW uplink beacon will have been transmitted from earth by the DSN to arrive at Pluto during spacecraft closest approach. Reflection from the specular zone is expected to be sufficiently strong to observe the bistatic uplink in the REX narrowband record. Measurements in both polarizations will then be combined to yield surface reflectivity, roughness and limits on the dielectric constant in the specular zone.

Three Views of Pluto

NASA Image and Video Library

2015-07-06

New Horizons' Long Range Reconnaissance Imager (LORRI) obtained these three images of Pluto between July 1-3 ,2015, as the spacecraft closed in on its July 14 encounter with the dwarf planet and its moons. The left image shows, on the right side of the disk, a large bright area on the hemisphere opposite Charon; this is the side of Pluto that will be seen in close-up by New Horizons on July 14. The three images together show the full extent of a continuous swath of dark terrain that wraps around Pluto's equatorial region between longitudes 40° and 160°. The western end of the swath, west of longitude 40°, breaks up into a series of striking dark regularly-spaced spots on the anti-Charon hemisphere (right image) that were first noted in New Horizons images taken on Pluto's previous rotation. Intriguing details are beginning to emerge in the bright material north of the dark region, in particular a series of bright and dark patches that are conspicuous just below the center of the disk in the right-hand image. In all three black-and-white views, the apparent jagged bottom edge of Pluto is the result of image processing. http://photojournal.jpl.nasa.gov/catalog/PIA19698

The Formation of Charon's Red Poles from Seasonally Cold-Trapped Volatiles

NASA Technical Reports Server (NTRS)

Grundy, W. M.; Cruikshank, D. P.; Gladstone, D. R.; Howett, C. J. A.; Lauer, T. R.; Spencer, J. R.; Summers, M. E.; Buie, M. W.; Earle, A. M.; Ennico, K.;

The formation of Charon's red poles from seasonally cold-trapped volatiles.

PubMed

Grundy, W M; Cruikshank, D P; Gladstone, G R; Howett, C J A; Lauer, T R; Spencer, J R; Summers, M E; Buie, M W; Earle, A M; Ennico, K; Parker, J Wm; Porter, S B; Singer, K N; Stern, S A; Verbiscer, A J; Beyer, R A; Binzel, R P; Buratti, B J; Cook, J C; Dalle Ore, C M; Olkin, C B; Parker, A H; Protopapa, S; Quirico, E; Retherford, K D; Robbins, S J; Schmitt, B; Stansberry, J A; Umurhan, O M; Weaver, H A; Young, L A; Zangari, A M; Bray, V J; Cheng, A F; McKinnon, W B; McNutt, R L; Moore, J M; Nimmo, F; Reuter, D C; Schenk, P M

2016-11-03

A unique feature of Pluto's large satellite Charon is its dark red northern polar cap. Similar colours on Pluto's surface have been attributed to tholin-like organic macromolecules produced by energetic radiation processing of hydrocarbons. The polar location on Charon implicates the temperature extremes that result from Charon's high obliquity and long seasons in the production of this material. The escape of Pluto's atmosphere provides a potential feedstock for a complex chemistry. Gas from Pluto that is transiently cold-trapped and processed at Charon's winter pole was proposed as an explanation for the dark coloration on the basis of an image of Charon's northern hemisphere, but not modelled quantitatively. Here we report images of the southern hemisphere illuminated by Pluto-shine and also images taken during the approach phase that show the northern polar cap over a range of longitudes. We model the surface thermal environment on Charon and the supply and temporary cold-trapping of material escaping from Pluto, as well as the photolytic processing of this material into more complex and less volatile molecules while cold-trapped. The model results are consistent with the proposed mechanism for producing the observed colour pattern on Charon.

Formation of the Sputnik Planum basin and the thickness of Pluto's subsurface ocean

NASA Astrophysics Data System (ADS)

Johnson, B. C.; Bowling, T.; Trowbridge, A.; Freed, A. M.

2016-12-01

Since the New Horizons flyby, evidence has been mounting that Pluto's Sputnik Planum (SP; informal name) (1,2) is associated with a 800-1000 km diameter elliptical impact basin (3,4). Global tectonics and the location of SP suggests that Pluto reoriented to align the basin with its tidal axis (4,5). This indicates there is a large positive mass anomaly associated with SP (4,5). However, even with loading of 3-10 km of dense convecting N2 ice (6,7), a positive mass anomaly associated with the deep basin requires that Pluto has a liquid ocean and the ice shell under the basin is substantially thinned (4). Although the possibility of a slowly freezing current day subsurface ocean is supported by thermal modeling (8,9) and the ubiquity of young extensional tectonic features (1), the thickness of the putative ocean is unconstrained. Here, we simulate the SP basin-forming impact into targets with a range of thermal states and ocean thicknesses. We find that SP can only achieve a large positive mass anomaly if Pluto has a more than 100 km thick salty ocean (i.e. ocean density exceeding 1100 kg/m3). This conclusion may help us better understand the composition and thermal evolution of Pluto. 1. Moore, J. M. et al. Science 351,1284-1293 (2016). 2. Stern, S. A. et al. Science 350,aad1815-aad1815 (2015). 3. Schenk, P. M. et al. A Large Impact Origin for Sputnik Planum and Surrounding Terrains, Pluto? AAS/Division for Planetary Sciences Meeting Abstracts 47,(2015). 4. Nimmo, F. et al. Loading, Relaxation, and Tidal Wander at Sputnik Planum, Pluto. 47th Lunar and Planetary Science Conference 47,2207 (2016). 5. Keane, J. T. & Matsuyama, I. Pluto Followed Its Heart: True Polar Wander of Pluto Due to the Formation and Evolution of Sputnik Planum. 47th Lunar and Planetary Science Conference 47,2348 (2016). 6. Trowbridge, A. J., Melosh, H. J., Steckloff, J. K. & Freed, A. M. Nature 534,79-81 (2016). 7. McKinnon, W. B. et al. Nature 534,82-85 (2016). 8. Robuchon, G. & Nimmo, F. Icarus 216,426-439 (2011). 9. Hammond, N. P., Barr, A. C. & Parmentier, E. M. Geophys. Res. Lett. (2016). doi:10.1002/2016GL069220

A Binary Planet in Color

NASA Image and Video Library

2015-07-23

This image from NASA New Horizons highlights the contrasting appearance of the two worlds: Charon is mostly gray, with a dark reddish polar cap, while Pluto shows a wide variety of subtle color variations. Pluto and Charon are shown in enhanced color in this image, which is the highest-resolution color image of the pair so far returned to Earth by New Horizons. It was taken at 06:49 UT on July 14, 2015, five hours before Pluto closest approach, from a range of 150,000 miles (250,000 kilometers), with the spacecraft's Ralph instrument. The image highlights the contrasting appearance of the two worlds: Charon is mostly gray, with a dark reddish polar cap, while Pluto shows a wide variety of subtle color variations, including yellowish patches on the north polar cap and subtly contrasting colors for the two halves of Pluto's "heart," informally named Tombaugh Regio, seen in the upper right quadrant of the image. In order to fit Pluto and Charon in the same frame in their correct relative positions, the image has been rotated so the north pole on both Pluto and Charon is pointing towards the upper left. The image was made with the blue, red, and near-infrared color filters of Ralph's Multispectral Visible Imaging Camera, and shows colors that are similar, but not identical, to what would be seen with the human eye, which is sensitive to a narrower range of wavelengths. http://photojournal.jpl.nasa.gov/catalog/PIA19856

New Horizons Very Best View of Pluto

NASA Image and Video Library

2015-12-05

This frame from a movie is composed of the sharpest views of Pluto that NASA's New Horizons spacecraft obtained during its flyby of the distant planet on July 14, 2015. The pictures are part of a sequence taken near New Horizons' closest approach to Pluto, with resolutions of about 250-280 feet (77-85 meters) per pixel -- revealing features smaller than half a city block on Pluto's diverse surface. The images include a wide variety of spectacular, cratered, mountainous and glacial terrains -- giving scientists and the public alike a breathtaking, super-high resolution window on Pluto's geology. The images form a strip 50 miles (80 kilometers) wide trending from Pluto's jagged horizon about 500 miles (800 kilometers) northwest of the informally named Sputnik Planum, across the al-Idrisi mountains, onto the shoreline of Sputnik Planum and then across its icy plains. They were made with the telescopic Long Range Reconnaissance Imager (LORRI) aboard New Horizons, over a timespan of about a minute centered on 11:36 UT on July 14 -- just about 15 minutes before New Horizons' closest approach to Pluto -- from a range of just 10,000 miles (17,000 kilometers). They were obtained with an unusual observing mode; instead of working in the usual "point and shoot," LORRI snapped pictures every three seconds while the Ralph/Multispectral Visual Imaging Camera (MVIC) aboard New Horizons was scanning the surface. This mode requires unusually short exposures to avoid blurring the images. http://photojournal.jpl.nasa.gov/catalog/PIA20202

New Horizons Very Best View of Pluto Mosiac

NASA Image and Video Library

2015-12-05

This mosaic is composed of the sharpest views of Pluto that NASA's New Horizons spacecraft obtained during its flyby of the distant planet on July 14, 2015. The pictures are part of a sequence taken near New Horizons' closest approach to Pluto, with resolutions of about 250-280 feet (77-85 meters) per pixel -- revealing features smaller than half a city block on Pluto's diverse surface. The images include a wide variety of spectacular, cratered, mountainous and glacial terrains -- giving scientists and the public alike a breathtaking, super-high resolution window on Pluto's geology. The images form a strip 50 miles (80 kilometers) wide trending from Pluto's jagged horizon about 500 miles (800 kilometers) northwest of the informally named Sputnik Planum, across the al-Idrisi mountains, onto the shoreline of Sputnik Planum and then across its icy plains. They were made with the telescopic Long Range Reconnaissance Imager (LORRI) aboard New Horizons, over a timespan of about a minute centered on 11:36 UT on July 14 -- just about 15 minutes before New Horizons' closest approach to Pluto -- from a range of just 10,000 miles (17,000 kilometers). They were obtained with an unusual observing mode; instead of working in the usual "point and shoot," LORRI snapped pictures every three seconds while the Ralph/Multispectral Visual Imaging Camera (MVIC) aboard New Horizons was scanning the surface. This mode requires unusually short exposures to avoid blurring the images. http://photojournal.jpl.nasa.gov/catalog/PIA20201

Pluto Close-up, Now in Color

NASA Image and Video Library

2015-12-10

This enhanced color mosaic combines some of the sharpest views of Pluto that NASA's New Horizons spacecraft obtained during its July 14 flyby. The pictures are part of a sequence taken near New Horizons' closest approach to Pluto, with resolutions of about 250-280 feet (77-85 meters) per pixel -- revealing features smaller than half a city block on Pluto's surface. Lower resolution color data (at about 2,066 feet, or 630 meters, per pixel) were added to create this new image. The images form a strip 50 miles (80 kilometers) wide, trending (top to bottom) from the edge of "badlands" northwest of the informally named Sputnik Planum, across the al-Idrisi mountains, onto the shoreline of Pluto's "heart" feature, and just into its icy plains. They combine pictures from the telescopic Long Range Reconnaissance Imager (LORRI) taken approximately 15 minutes before New Horizons' closest approach to Pluto, with -- from a range of only 10,000 miles (17,000 kilometers) -- with color data (in near-infrared, red and blue) gathered by the Ralph/Multispectral Visible Imaging Camera (MVIC) 25 minutes before the LORRI pictures. The wide variety of cratered, mountainous and glacial terrains seen here gives scientists and the public alike a breathtaking, super-high-resolution color window into Pluto's geology. e border between the relatively smooth Sputnik Planum ice sheet and the pitted area, with a series of hills forming slightly inside this unusual "shoreline." http://photojournal.jpl.nasa.gov/catalog/PIA20213

Research on automated disassembly technology for waste LCD

NASA Astrophysics Data System (ADS)

Qin, Qin; Zhu, Dongdong; Wang, Jingwei; Dou, Jianfang; Wang, Sujuan; Tu, Zimei

2017-11-01

In the field of Waste LCD disassembling and recycling, there are existing two major problems: 1) disassembling waste LCD mainly depends on manually mechanical crushing; 2) the resource level is not high. In order to deal with the above problems, in this paper, we develop an efficient, safe and automated waste LCD disassembling assembly line technology. This technology can disassembly and classify mainstream LCD into four components, which are liquid crystal display panels, housings and metal shield, PCB assembly. It can also disassembly many kinds of waste LCD. Compared with the traditional cooperation of manual labor and electric tools method, our proposed technology can significantly improve disassembling efficiency and demonstrate good prospects and promotional value.

Double Planet Meets Triple Star

NASA Astrophysics Data System (ADS)

2002-08-01

High-Resolution VLT Image of Pluto Event on July 20, 2002 A rare celestial phenomenon involving the distant planet Pluto has occurred twice within the past month. Seen from the Earth, this planet moved in front of two different stars on July 20 and August 21, respectively, providing observers at various observatories in South America and in the Pacific area with a long awaited and most welcome opportunity to learn more about the tenuous atmosphere of that cold planet. On the first date, a series of very sharp images of a small sky field with Pluto and the star was obtained with the NAOS-CONICA (NACO) adaptive optics (AO) camera mounted on the ESO VLT 8.2-m YEPUN telescope at the Paranal Observatory. With a diameter of about 2300 km, Pluto is about six times smaller than the Earth. Like our own planet, it possesses a relatively large moon, Charon , measuring 1200 km across and circling Pluto at a distance of about 19,600 km once every 6.4 days. In fact, because of the similarity of the two bodies, the Pluto-Charon system is often referred to as a double planet . At the current distance of nearly 4,500 million km from the Earth, Pluto's disk subtends a very small angle in the sky, 0.107 arcsec. It is therefore very seldom that Pluto - during its orbital motion - passes exactly in front of a comparatively bright star. Such events are known as "occultations" , and it is difficult to predict exactly when and where on the Earth's surface they are visible. Stellar occultations When Pluto moves in front of a star, it casts a "shadow" on the Earth's surface within which an observer cannot see the star, much like the Earth's Moon hides the Sun during a total solar eclipse. During the occultation event, Pluto's "shadow" also moves across the Earth's surface. The width of this shadow is equal to Pluto's diameter, i.e. about 2300 km. One such occultation event was observed in 1988, and two others were expected to occur in 2002, according to predictions published in 2000 by American astronomers Steve W. McDonald and James L. Elliot (Massachussetts Institute of Technology [MIT], Cambridge, USA). Further refinements provided by other observers later showed that the first event would be visible from South America on July 20, 2002 , while a second one on August 21 was expected to be observable in the Pacific basin, from the western coast of North America down to Hawaii and New Zealand. A stellar occultation provides a useful opportunity to study the planetary atmosphere, by means of accurate photometric measurements of the dimming of the stellar light, as the planet moves in front of the star. The observed variation of the light intensity and colour provides crucial information about the structure (atmospheric layers) and composition of different gases and aerosols. More information is available in the Appendix below. The July 20 occultation ESO PR Photo 21a/02 ESO PR Photo 21a/02 [Preview - JPEG: 400 x 477 pix - 65k] [Normal - JPEG: 800 x 953 pix - 224k] Caption : PR Photo 21c/02 shows the path of Pluto's shadow (grey region) during the July 20, 2002 occultation. The shadow has a diameter of about 2300 km and moves from right to left; the timings along the central line are indicated in one-minute intervals (Universal Time - UT). The width of the gray area corresponds to the regions where more than 50% of the light from the star P126 A was attenuated by Pluto's atmosphere. The dotted lines indicate where the stellar flux was attenuated by more than 10%. The maximum duration of the occultation (for observers located at the middle of the shadow track) was about 3 min. The plot is based on astrometric measurements posted at the MIT site. Once completely analyzed, the VLT NACO images will provide significantly better accuracy on the location of this track and therefore a solid basis for the interpretation of the photometric observations obtained with other telescopes. In order to profit from the rare opportunity to learn more about Pluto and its atmosphere, a large campaign involving more than twenty scientists and engineers from the Paris Observatory and associated institutions [1] was organized to observe the July 20, 2002, event involving an occultation of a star of visual magnitude 11 (i.e., about 100 times fainter than what can be perceived with then unaided eye), referred to as "P126" in McDonald and Elliot's catalogue. In May 2002, preparatory observations showed that star to be double, with the brighter component of the system ( "P126 A" ) being likely to be occulted by Pluto, as seen from South America. However, because of the duplicity, the predictions of exactly where the shadow of Pluto would sweep the ground were uncertain by about 0.1 arcsec in the sky, corresponding to more than 2000 km on the ground. The NACO images ESO PR Photo 21b/02 ESO PR Photo 21b/02 [Preview - JPEG: 400 x 469 pix - 47k] [Normal - JPEG: 800 x 937 pix - 208k] ESO PR Photo 21c/02 ESO PR Photo 21c/02 [Preview - JPEG: 400 x 467 pix - 53k] [Normal - JPEG: 800 x 933 pix - 232k] Caption : PR Photo 21b/02 shows one of the images obtained with the NAOS-CONICA (NACO) adaptive optics (AO) camera mounted on the ESO VLT 8.2-m YEPUN telescope at the Paranal Observatory in connection with a stellar occultation by Pluto on July 20, 2002. The star was found to be triple - the three components (A, B and C), as well as Pluto and its moon, Charon, are indicated in PR Photo 21c/02 for easy orientation. The images are based on data available from the NACO data webpage. See the text for details. In the end, the close approach (an "appulse" in astronomical terminology) of Pluto and P126 A was indeed observed from various sites in South America, with several mobile telescopes and also including major facilities at the ESO La Silla and Paranal Observatories. In particular, unique and very sharp images were obtained with the NAOS-CONICA (NACO) adaptive optics (AO) camera mounted on the ESO VLT 8.2-m YEPUN telescope . One of the NACO images is shown in PR Photos 21b-c/02 . These images were made during the final adjustments of the NACO instrument and in anticipation of the upcoming science verification observations. All frames are now publicly available from the NACO data webpage on the ESO site. The NACO image shown was obtained in infrared light (in the K-band at wavelength 2.2 µm) on July 20, 2002, some 45 min before Pluto's shadow passed north of Paranal ( Photo 21a/02) . The orientation is such that North is up, and East is left. The small sky field measures about 7 x 7 arcsec 2. The pixel size is 0.027 arcsec, and the achieved image sharpness corresponds to the theoretical limit (the diffraction limit) with a telescope of this size and at this wavelength (0.07 arcsec). The object at the centre is the star P126 A of K-magnitude 9.5 (see also Photo 21c/02 where the objects are identified), while the brighter object at the right is the companion star P126 B , 2.25 arcsec away. As P126 B is very red (of stellar type M), it appears brighter than P126 A at this infrared wavelength - the opposite is true in visible light. The intensity of the left part of the image has been multiplied by a factor of approximately 35 in order to better display Pluto and its moon Charon , located some 0.5 arcsec to the lower left (SE) of the planet. Note also the faint star "P126 C" , at this moment very close to Pluto; it is probably a (physical) member of the P126 system. A closer inspection of the original image shows that the disk of Pluto (with a diameter of 0.107 arscec and covering 16 NACO pixels) is (barely) resolved. Many images were taken by NACO prior to the occultation. They will allow to retrace the precise motion of Pluto relative to P126 A, thereby improving the mapping of the motion of Pluto's shadow on the ground, cf. Photo 21a/02 . This is important in order to apply the correct geometrical circumstances for the interpretation of the photometric observations. A first evaluation of the NACO data indicates that the Paranal site "missed" the upper layers of Pluto's atmosphere by a mere 200 km or so - this is equivalent to no more than one hundredth of an arcsec as projected on the sky. More information A full report on the NACO observations and other results by the present group of astronomers, also from the subsequent occultation of another star on August 21, 2002, that was extensively observed with the Canada-France-Hawaii Telescope (CFHT) on Mauna Kea (Hawaii, USA), is available at this URL: http://despa.obspm.fr/~sicardy/pluton/results.html Other sharp NACO images have been published recently, e.g. ESO PR 25/01 , ESO PR Photos 04a-c/02 and ESO PR Photos 19a-c/02. Note [1]: The group from the Observatoire de Paris and other observatories is lead by Bruno Sicardy and also includes François Colas, Thomas Widemann, Françoise Roques, Christian Veillet, Jean-Charles Cuillandre, Wolfgang Beisker, Cyril Birnbaum, Kate Brooks, Audrey Delsanti, Pierre Drossart, Agnès Fienga, Eric Gendron, Mike Kretlow, Anne-Marie Lagrange, Jean Lecacheux, Emmanuel Lellouch, Cédric Leyrat, Alain Maury, Elisabeth Raynaud, Michel Rapaport, Stefan Renner and Mathias Schultheis . From ESO participated Nancy Ageorges, Olivier Hainaut, Chris Lidman and Jason Spyromilio . Contact Bruno Sicardy LESIA - Observatoire de Paris France Phone: +33-1-45 07 71 15 email: bruno.sicardy@obspm.fr Appendix: Stellar occultations and Pluto's atmosphere Stellar occultations are presently the only way to probe Pluto's tenuous atmosphere . When the star moves behind the planet, the stellar rays suffer minute deviations as they are refracted (i.e., bent and defocussed) by the planet's atmospheric layers. This effect, together with the large distance to the planet, manifests itself as a gradual decline of observed intensity of the stellar light, rather than an abrupt drop as this would be the case if the planet had no atmosphere. Pluto's atmosphere was first detected on August 19, 1985, during a stellar occultation observed from Israel and then studied in more detail from Australia and from the Kuiper Airborne Observatory (KAO) during another such event on July 9, 1988. However, Pluto's atmosphere is still not well understood. It appears to be mostly composed of a dominant gas of atomic weight 28, probably molecular nitrogen (N 2 ). Near-IR solar reflection spectra have since shown a small presence of methane (CH 4 ), probably at a level of about 1% relative to nitrogen. The 1988 occultation clearly revealed two different layers in Pluto's atmosphere, a rather smooth and isothermal outer part, and a more complex one near the planet's surface, with the possible presence of an inversion layer (in which the temperature increases with altitude) or possibly haze of photochemical origin. The present observations aimed at discriminating between the current theoretical models of Pluto's atmosphere by means of detailed measurements of the changing intensity and colour of the stellar light, as the star is seen through progressively lower layers of the planet's atmosphere. Another important issue is the question of whether Pluto's atmosphere has changed since 1988. In the intervening 14 years, the planet has moved away from the Sun in its elliptic orbit, whereby there has been a change in the insolation (solar flux) of about 6%. This effect might possibly have caused changes in the surface temperature and in the overall atmospheric structure of Pluto. However, any firm conclusions will have to await a complete and careful evaluation of all available observations. ESO PR Photos 21a-c/02 may be reproduced, if credit is given to the European Southern Observatory (ESO).

Detection of Atmospheric CO on Pluto with ALMA

NASA Astrophysics Data System (ADS)

Gurwell, Mark; Lellouch, Emmanuel; Butler, Bryan; Moullet, Arielle; Moreno, Raphael; Bockelée-Morvan, Dominique; Biver, Nicolas; Fouchet, Thierry; Lis, Darek; Stern, Alan; Young, Leslie; Young, Eliot; Weaver, Hal; Boissier, Jeremie; Stansberry, John

2015-11-01

We observed Pluto and Charon using the Atacama Large Millimeter/submillimeter Array (ALMA) interferometer in Northern Chile on June 12.2 and June 13.15, 2015, just one month prior to the New Horizons flyby of the system. The configuration of ALMA at the time provided ~0.3" resolution, allowing separation of emission from Pluto and Charon. This project targeted multiple science goals, including a search for HCN in Pluto's atmosphere [1] and high precision measurements of the individual brightness temperatures of Pluto and Charon [2], also presented at this meeting. Here we report the high SNR detection of carbon monoxide in the atmosphere of Pluto. The CO(3-2) rotational line, at 345.796 GHz (867 μm), was observed with 117 kHz spectral resolution for 45 min (on-source) on each date, providing ~3.5mJy/channel RMS. CO emission was clearly detected on both days, with a contrast of ~65 mJy above the Pluto continuum, and ~1.8 MHz FWHM linewidth, with the combined integrated line SNR >50. The presence of CO in Pluto's atmosphere is expected due to it's presence as ice on the surface in vapor pressure equilibrium with the atmosphere (e.g. [3],[4]), and it was previously detected at modest SNR in the near-IR using the VLT [5]. A preliminary assessment based upon the CO line wings shows the fractional abundance of CO is 500-750 ppm, consistent with that found in [5]. Further, the shape of the line core emission (assuming a constant CO mixing ratio), suggests that the atmospheric temperature rises quickly from the surface to ~100-110 K in the altitude range 20-70 km but decreases above that, falling to about 70 K by 200 km altitude. A detailed line inversion analysis will be performed and results presented.[1] Lellouch et al, this meeting. [2] Butler et al., this meeting. [3] Owen et al (1993), Science, 261, pp. 745-748. [4] Spencer et al (1993), In Pluto and Charon, pp. 435-473. Univ. of Arizona Press, Tucson. [5] Lellouch et al (2011), A&A, 530, L4.

Modeling Low Velocity Impacts: Predicting Crater Depth on Pluto

NASA Astrophysics Data System (ADS)

Bray, V. J.; Schenk, P.

2014-12-01

The New Horizons mission is due to fly-by the Pluto system in Summer 2015 and provides the first opportunity to image the Pluto surface in detail, allowing both the appearance and number of its crater population to be studied for the first time. Bray and Schenk (2014) combined previous cratering studies and numerical modeling of the impact process to predict crater morphology on Pluto based on current understanding of Pluto's composition, structure and surrounding impactor population. Predictions of how the low mean impact velocity (~2km/s) of the Pluto system will influence crater formation is a complex issue. Observations of secondary cratering (low velocity, high angle) and laboratory experiments of impact at low velocity are at odds regarding how velocity controls depth-diameter ratios: Observations of secondary craters show that these low velocity craters are shallower than would be expected for a hyper-velocity primary. Conversely, gas gun work has shown that relative crater depth increases as impact velocity decreases. We have investigated the influence of impact velocity further with iSALE hydrocode modeling of comet impact into Pluto. With increasing impact velocity, a projectile will produce wider and deeper craters. The depth-diameter ratio (d/D) however has a more complex progression with increasing impact velocity: impacts faster than 2km/s lead to smaller d/D ratios as impact velocity increases, in agreement with gas-gun studies. However, decreasing impact velocity from 2km/s to 300 m/s produced smaller d/D as impact velocity was decreased. This suggests that on Pluto the deepest craters would be produced by ~ 2km/s impacts, with shallower craters produced by velocities either side of this critical point. Further simulations to investigate whether this effect is connected to the sound speed of the target material are ongoing. The complex relationship between impact velocity and crater depth for impacts occurring between 300m/s and 10 km/s suggests that there might be a larger range of 'pristine' crater depths on Pluto than on bodies with higher mean impact velocity. This might affect our ability to define a pristine crater depth as a starting point for crater infill and relaxation studies.

The Pluto System At Small Phase Angles

NASA Astrophysics Data System (ADS)

Verbiscer, Anne J.; Buie, Marc W.; Binzel, Richard; Ennico, Kimberly; Grundy, William M.; Olkin, Catherine B.; Showalter, Mark Robert; Spencer, John R.; Stern, S. Alan; Weaver, Harold A.; Young, Leslie; New Horizons Science Team

2016-10-01

Hubble Space Telescope observations of the Pluto system acquired during the New Horizons encounter epoch (HST Program 13667, M. Buie, PI) span the phase angle range from 0.06 to 1.7 degrees, enabling the measurement and characterization of the opposition effect for Pluto and its satellites at 0.58 microns using HST WFC3/UVIS with the F350LP filter, which has a broadband response and a pivot wavelength of 0.58 microns. At these small phase angles, differences in the opposition effect width and amplitude appear. The small satellites Nix and Hydra both exhibit a very narrow opposition surge, while the considerably larger moon Charon has a broader opposition surge. Microtextural surface properties derived from the shape and magnitude of the opposition surge of each surface contain a record of the collisional history of the system. We combine these small phase angle observations with those made at larger phase angles by the New Horizons Long Range Reconnaissance Imager (LORRI), which also has a broadband response with a pivot wavelength of 0.61 microns, to produce the most complete disk-integrated solar phase curves that we will have for decades to come. Modeling these disk-integrated phase curves generates sets of photometric parameters that will inform spectral modeling of the satellite surfaces as well as terrains on Pluto from spatially resolved New Horizons Ralph Linear Etalon Imaging Spectral Array (LEISA) data from 1.2 to 2.5 microns. Rotationally resolved phase curves of Pluto reveal opposition effects that only appear at phase angles less than 0.1 degree and have widths and amplitudes that are highly dependent on longitude and therefore on Pluto's diverse terrains. The high albedo region informally known as Sputnik Planum dominates the disk-integrated reflectance of Pluto on the New Horizons encounter hemisphere. These results lay the groundwork for observations at true opposition in 2018, when the Pluto system will be observable at phase angles so small that an Earth transit across the solar disk will be visible from Pluto and its satellites.

Geology and Composition of Pluto and Charon from New Horizons

NASA Astrophysics Data System (ADS)

Spencer, John R.; Stern, S. Alan; Moore, Jeffrey M.; Grundy, W. M.; McKinnon, William B.; Cruikshank, Dale P.; Weaver, Harold A.; Olkin, Catherine B.; Young, Leslie; Ennico, Kimberly; New Horizons Geology/Geophysics and Composition Theme Teams

2016-10-01

Data gathered by New Horizons during its July 2015 flyby has revolutionized our understanding of the geology and surface composition of Pluto and Charon. While much of Pluto's ice shell is ancient and rigid, as evinced by locally high crater densities and deep graben, much of the surface has been reworked, up to the present day, by a bewildering variety of geological processes. These include deposition and erosion of kilometers of mantle material, sublimation, apparent cryovolcanism, chaotic breakup of the crust to form rugged mountains, erosion and creation of channel networks by probable glacial action, and active glaciation. Pluto's anti-Charon hemisphere is dominated by 1000 km wide field of actively convecting nitrogen and other ices, informally called Sputnik Planum, occupying a large depression of probable impact origin. Color and composition is very varied, and is dominated by dark red tholins and N2, CH4, and CO ices, with H2O ice bedrock also exposed in many places. Apart from Sputnik Planum, color and composition is strongly correlated with latitude, showing the importance of insolation in controlling ice distribution. Charon shows pervasive extensional tectonism and locally extensive cryovolcanic resurfacing, both dating from early in solar system history. Its color and surface composition, dominated by H2O ice plus NH3 hydrate, is remarkably uniform apart from a thin deposit of dark red material near the north pole which may be due to cold-trapping and radiolysis of hydrocarbons escaping from Pluto. Neither Pluto nor Charon is likely to have experienced tidal heating during the period when observable landforms were created. Charon's surface shows resurfacing comparable in extent and age to many Saturnian and Uranian satellites such as Dione or Ariel, suggesting that observed activity on these satellites may not necessarily be tidally-driven. Pluto demonstrates that resurfacing on small volatile-rich icy bodies can be powered for at least 4.5 Ga by ongoing radiogenic and residual early heat alone, though the fact that Triton shows much more pervasive resurfacing than Pluto provides some evidence that Triton, unlike Pluto, has access to an additional heat source, presumably tidal.

Cosmogonic constraints from densities in the Pluto system and rotational and tidal figures of equilibrium for Pluto and Charon

NASA Astrophysics Data System (ADS)

McKinnon, W.; Buie, M.; Moore, J.; Linscott, I.; Hinson, D.; Tyler, G.; Singer, K.; Stern, S.; New Horizons Team

2014-07-01

A byproduct of the discovery of Nix, Hydra, Styx, and Kerberos, and the detailed study of their orbits, has been a relatively precise determination of the system barycenter, and thus the Pluto/Charon mass ratio [1]. Coupled with precise determinations of Charon's size by multiple stellar occultations [2,3], Charon's mean density is now relatively well-determined (1.72 ± 0.02 g cm^{-3}), both in an absolute sense and with respect to that of Pluto (1.89 ± 0.06 g cm^{-3}) [1]. The latter's precise size remains uncertain due to the effects of its atmosphere on stellar occultations [e.g., 4] and of limb darkening on mutual events [5]. Both Pluto and Charon are relatively rock-rich, but Charon is somewhat icier, which is consistent with impact origin scenarios in which one or both precursor bodies were at least partially differentiated (rock separated from ice under the action of gravity) [6,7]. Ice-rich ejecta is also the preferred route for forming a particle disk outside of Charon's initial post-giant-impact orbit, such as would lead to accretion of the small satellites [8]. In this regard, the upper limits on the densities of the brightest and presumably largest of the small satellites (Nix and Hydra) are - even at the 3σ level -- consistent with very icy and porous bodies. Icy rubble-pile bodies are predicted by the initial conditions of the giant impact as presently understood (conditions necessary to give an icier Charon). The small satellites will thus offer an interesting cosmogonical test during the 14 July 2015 New Horizons encounter, as good constraints will be placed on satellite volumes from imaging and improved satellite masses should result from optical navigation and orbital simulations. The fly-through of the Pluto-Charon system by New Horizons also offers the first opportunity to determine both the total system mass and the individual masses of Pluto and Charon by direct Doppler tracking (although the spacecraft will not pass close enough to any of the small satellites to measure their gravitational accelerations). Simulations of the encounter by the REX Radio Science experiment indicate the potential accuracies of the combined and individual mass determinations of Pluto and Charon are on the order of 0.1 % [9,10], a substantial improvement in precision (especially for Charon). This will put to rest a long-standing limitation on modeling and understanding Pluto and Charon's internal structure and evolution [11]. It is notable, from the densities quoted above, that the ''density gap'' between Pluto and Charon appears to be narrowing, and at the 3σ level and considering the effects of porosity, this gap could even be zero. If Pluto and Charon were close in density after all, it could change our view as to how the binary formed [12]. Refinement at the next level, that is, determining Pluto's or Charon's internal structure, specifically their degree of differentiation (or even the presence or absence of oceans), will not be easy. New Horizons will not pass close enough to measure the degree-2 gravity field for either body (nor was such an original measurement requirement or mission objective), but shape determination from imaging offers the possibility of determining differentiation state. For this to be successful, however, Pluto or Charon must be in hydrostatic equilibrium. For all hydrostatic models of these two bodies, the differences between the lengths of the principal axes of their figures are predicted to be less than 1 km, and the differences between differentiated and undifferentiated models smaller still [13]. Thus, discriminating between the two cases will be challenging. Furthermore, either Pluto or Charon may choose not to cooperate, if they retain fossil hydrostatic figures from earlier in their mutual tidal evolution [14], in the manner of Iapetus [e.g., 15]. These fossil figures would be larger (more biaxial in the case of Pluto, and more triaxial for Charon), and thus much easier to measure, and could provide important clues to Pluto's thermal and structural evolution [16].

Posttest examination of Sodium Loop Safety Facility experiments. [LMFBR

DOE Office of Scientific and Technical Information (OSTI.GOV)

Holland, J.W.

In-reactor, safety experiments performed in the Sodium Loop Safety Facility (SLSF) rely on comprehensive posttest examinations (PTE) to characterize the postirradiation condition of the cladding, fuel, and other test-subassembly components. PTE information and on-line instrumentation data, are analyzed to identify the sequence of events and the severity of the accident for each experiment. Following in-reactor experimentation, the SLSF loop and test assembly are transported to the Hot Fuel Examination Facility (HFEF) for initial disassembly. Goals of the HFEF-phase of the PTE are to retrieve the fuel bundle by dismantling the loop and withdrawing the test assembly, to assess the macro-conditionmore » of the fuel bundle by nondestructive examination techniques, and to prepare the fuel bundle for shipment to the Alpha-Gamma Hot Cell Facility (AGHCF) at Argonne National Laboratory.« less

The 19th of July 2016 Multi-Chord Stellar Occultation by Pluto - A European PRO-AM cooperation

NASA Astrophysics Data System (ADS)

Beisker, W.; Eberle, A.; Gaehrken, B.; Kattentidt, B.; Murawski, G.; Gazeas, K.; Tzouganatos, L.; Tigani, K.; Gloistein, D.; Hampf, D.; Hampf, D.; Eichler, H.; Hattenbach, J.; Guhl, K.; Dohrmann, M.; Krannich, G.; Lindner, P.; Marchini, A.; Papini, R.; Salvaggio, F.; Ohlert, J.; Kloes, O.; Farago, O.; Farago, A.; Grzedzielsk, P.; Signoret, F.; Moravec, Z.; Tsamis, V.; Wortmann, G.; Walzel, K.; Rothe, W.; Bode, H.-J.; Dangl, G.; Berard, D.; Desmars, J.; Leiva, R.; Meza, E.; Assafin, M.; Benedetti-Rossi, G.; Braga Ribas, F.; Camargo, J.; Dias de Oliveira, A.; Gomes Junior, A.; Vieira, R. M.; Ortiz, J. L.; Duffard, R.; Santos-Sanz, P.; Morales, N.; Sicardy, B.

2017-09-01

The occultation of the 14th mag star UCAC4 345-180315 by Pluto on the evening of the 19th of July, 2016 could be observed from large parts of Europe, middle east and northern Africa as well. A campaign had been organized with for many observers and observatories throughout Europe and other countries. Professional as well as amateur observatories and observers shared in a PRO-AM cooperation to achieve the highest possible degree of coverage. The scientific goal was the ongoing monitoring of Pluto's atmosphere, waiting for a possible shrinking of its pressure due to the increasing distance of Pluto from the sun.

Pluto-Charon: Infrared Reflectance from 3.6 to 8.0 Micrometers

NASA Technical Reports Server (NTRS)

Cruikshank, Dale P.; Emery, Joshua P.; Stansberry, John A.; VanCleve, Jeffrey E.

2004-01-01

We have measured the spectral reflectance of the Pluto-Charon pair at 3.6, 4.5, 5.8, and 8.0 micrometers with the Infrared Array Camera (IRAC) (G. G. Fazzio et al. Ap.J.Supp. 154, 10-17, 2004) on the Spitzer Space Telescope (STS), at eight different longitudes that cover a full rotation of the planet. STS does not have sufficient resolution to separate the light from the planet and the satellite. The image of the Pluto-Charon pair is clearly visible at each of the four wavelengths. We will discuss the spectral reflectance in terms of models that include the known components of Pluto and Charon s surfaces, and evidence for diurnal variations.

NASA Missions Have Their Eyes Peeled on Pluto Artist Concept

NASA Image and Video Library

2015-07-09

This artist concept shows NASA fleet of observatories busily gathering data before and after July 14, 2015 to help piece together what we know about Pluto, and what features New Horizons data might help explain. What's icy, has "wobbly" potato-shaped moons, and is arguably the world's favorite dwarf planet? The answer is Pluto, and NASA's New Horizons is speeding towards the edge of our solar system for a July 14 flyby. It won't be making observations alone; NASA's fleet of observatories will be busy gathering data before and after to help piece together what we know about Pluto, and what features New Horizons data might help explain. http://photojournal.jpl.nasa.gov/catalog/PIA19703

29 CFR 1926.1407 - Power line safety (up to 350 kV)-assembly and disassembly.

Code of Federal Regulations, 2011 CFR

2011-07-01

... 29 Labor 8 2011-07-01 2011-07-01 false Power line safety (up to 350 kV)-assembly and disassembly... Cranes and Derricks in Construction § 1926.1407 Power line safety (up to 350 kV)—assembly and disassembly... area of assembly/disassembly, closer than 20 feet to a power line during the assembly/disassembly...

Mass Determination of Pluto and Charon from New Horizon REX Radio Science Observations

NASA Astrophysics Data System (ADS)

Paetzold, Martin; Andert, T. P.; Tyler, G.; Bird, M. K.; Hinson, D. P.; Linscott, I. R.

2013-10-01

The anticipated 14 July 2015 New Horizons fly-through of the Pluto system provides the first opportunity to determine both the total system mass and the individual masses of Pluto and Charon by direct observation. This will be accomplished by use of: i) two-way Doppler radio frequency tracking data during intervals along the fly-in and -out trajectory, and ii) one-way uplink Doppler frequency recorded by the on-board radio science instrument, REX, during the day of closest approaches to Pluto and Charon. Continuous tracking is not feasible as a result of pointing sharing with the instruments during the encounter phase. Needed radio tracking will be obtained during time slots shared with i) two-way Doppler tracking for navigation, ii) 'plasma rolls' with the spacecraft antenna pointing to Earth, and iii) during the ingress and egress phases of the occultations. Simulations of the NH encounter indicate the potential accuracies of the combined and individual mass determinations of Pluto and Charon in the order of 0.1%.

Determination of the System Mass and the Individual Masses of the Pluto System from New Horizons Radio Tracking

NASA Astrophysics Data System (ADS)

Hahn, Matthias; Pätzold, Martin; Andert, Tom; Bird, Michael K.; Tyler, Leonard G.; Linscott, Ivan; Hinson, Dave P.; Stern, Alan; Weaver, Hal; Olkin, Cathrin; Young, Leslie; Ennico, Kimberly

2015-11-01

One objective of the New Horizons Radio Science Experiment REX is the determination of the system mass and the individual masses of Pluto and Charon. About four weeks of two-way radio tracking centered around the closest approach of New Horizons to the Pluto system were processed. Major problems during the processing were caused by the small net forces of the spacecraft thruster activity, which produce extra Δv on the spacecraft motion superposed onto the continuously perturbed motion caused by the attracting forces of the Pluto system. The times of spacecraft thruster activity are known but the applied Δv needs to be specifically adjusted. No two-way tracking was available for the day of the flyby, but slots of REX one-way uplink tracking are used to cover the most important times near closest approach, e.g. during occultation entries and exits. This will help to separate the individual masses of Pluto and Charon from the system mass.

Mass Determination of Pluto and Charon from New Horizon REX Radio Science Observations

NASA Astrophysics Data System (ADS)

Pätzold, M.; Andert, T. P.; Tyler, G. L.; Bird, M. K.; Hinson, D. H.; Linscott, I. R.

2013-09-01

The anticipated 14 July 2015 New Horizons flythrough of the Pluto system provides the first opportunity to determine both the total system mass and the individual masses of Pluto and Charon by direct observation. This will be accomplished by use of: i) two-way Doppler radio frequency tracking data during intervals along the fly-in and -out trajectory, and ii) one-way uplink Doppler frequency recorded by the on-board radio science instrument, REX, during the day of closest approaches to Pluto and Charon. Continuous tracking is not feasible as a result of pointing sharing with the instruments during the encounter phase. Needed radio tracking will be obtained during time slots shared with i) two-way Doppler tracking for navigation, ii) 'plasma rolls' with the spacecraft antenna pointing to Earth, and iii) during the ingress and egress phases of the occultations. Simulations of the NH encounter indicate the potential accuracies of the combined and individual mass determinations of Pluto and Charon in the order of 0.1%.

New Horizons Sees Pluto (Animation) Note: There is debate within the science community as to whether

NASA Technical Reports Server (NTRS)

2007-01-01

The Long Range Reconnaissance Imager (LORRI) on New Horizons acquired images of the Pluto field three days apart in late September 2006, in order to see Pluto's motion against a dense background of stars. LORRI took three frames at 1-second exposures on both Sept. 21 and Sept. 24. Because it moved along its predicted path, Pluto was detected in all six images.

These images are displayed using false-color to represent different intensities: the lowest intensity level is black, different shades of red mark intermediate intensities, and the highest intensity is white.

The images appear pixilated because they were obtained in a mode that compensates for the drift in spacecraft pointing over long exposure times. LORRI also made these observations before operators uploaded new flight-control software in October; the upgraded software package includes an optical navigation capability that will make LORRI approximately three times more sensitive still than for these Pluto observations.

A Close Look At Pluto

NASA Image and Video Library

2016-02-25

Pluto has long been a mystery, a dot at our solar system’s margins. The best images, even with NASA’s Hubble Space Telescope, were fuzzy and pixelated. In July 2015, NASA’s New Horizons spacecraft flew past Pluto and captured the sharpest views of the dwarf planet to date. One of the most striking areas, informally named "Sputnik Planum," is a sweeping, frozen plain the size of Texas and ringed by mountains of ice. Its smooth deposits are unmarred by impact craters, a stark contrast to the rest of Pluto’s battered surface. As a result, scientists believe the region formed recently, within the last few hundred million years. This contradicts past depictions of Pluto as an unchanging world. By analyzing images taken during the flyby, scientists hope to unravel more of the dwarf planet’s history. Watch the video for an up-close look at Pluto. Credit: NASA's Goddard Space Flight Center Video courtesy of NASA/Johns Hopkins University Applied Physics Laboratory/Southwest Research Institute/S. Robbins

Configuration of Pluto's Volatile Ices

NASA Astrophysics Data System (ADS)

Grundy, William M.; Binzel, R. P.; Cook, J. C.; Cruikshank, D. P.; Dalle Ore, C. M.; Earle, A. M.; Ennico, K.; Jennings, D. E.; Howett, C. J. A.; Linscott, I. R.; Lunsford, A. W.; Olkin, C. B.; Parker, A. H.; Parker, J. Wm; Protopapa, S.; Reuter, D. C.; Singer, K. N.; Spencer, J. R.; Stern, S. A.; Tsang, C. C. C.; Verbiscer, A. J.; Weaver, H. A.; Young, L. A.; Berry, K.; Buie, M. W.; Stansberry, J. A.

2015-11-01

We report on near-infrared remote sensing by New Horizons' Ralph instrument (Reuter et al. 2008, Space Sci. Rev. 140, 129-154) of Pluto's N2, CO, and CH4 ices. These especially volatile ices are mobile even at Pluto's cryogenic surface temperatures. Sunlight reflected from these ices becomes imprinted with their characteristic spectral absorption bands. The detailed appearance of these absorption features depends on many aspects of local composition, thermodynamic state, and texture. Multiple-scattering radiative transfer models are used to retrieve quantitative information about these properties and to map how they vary across Pluto's surface. Using parameter maps derived from New Horizons observations, we investigate the striking regional differences in the abundances and scattering properties of Pluto's volatile ices. Comparing these spatial patterns with the underlying geology provides valuable constraints on processes actively modifying the planet's surface, over a variety of spatial scales ranging from global latitudinal patterns to more regional and local processes within and around the feature informally known as Sputnik Planum. This work was supported by the NASA New Horizons Project.

The Pluto Case and the Nature of Science

NASA Astrophysics Data System (ADS)

Nóbrega de Albuquerque, Vanessa; Leite, Cristina

2016-08-01

Pluto had its classification changed in 2006, from planet to “dwarf planet”. This change had great impact in the media. Pluto returned to the news due to the arrival of New Horizons probe to Pluto in July 2015. Whereas the understanding of the complexity involved in the definition of celestial bodies could help us to show science as a historic, social, collective, non-linear and non-neutral process, it is presented a historical survey of the episodes involving the various definitions for planet, since the first observations of the sky made by our ancestors until the resolutions that defined which are the attributes of a "planet " made at the 26th General Assembly of the International Astronomical Union, meeting at which it was decided to reclassify Pluto. In order contribute to help perform discussions about the nature of science involving Astronomy themes, it is explained which features of scientific knowledge become evident during the study of the mentioned episodes.

Revisiting the 1988 Pluto Occultation

NASA Astrophysics Data System (ADS)

Bosh, Amanda S.; Dunham, Edward W.; Young, Leslie A.; Slivan, Steve; Barba née Cordella, Linda L.; Millis, Robert L.; Wasserman, Lawrence H.; Nye, Ralph

2015-11-01

In 1988, Pluto's atmosphere was surmised to exist because of the surface ices that had been detected through spectroscopy, but it had not yet been directly detected in a definitive manner. The key to making such a detection was the stellar occultation method, used so successfully for the discovery of the Uranian rings in 1977 (Elliot et al. 1989; Millis et al. 1993) and before that for studies of the atmospheres of other planets.On 9 June 1988, Pluto occulted a star, with its shadow falling over the South Pacific Ocean region. One team of observers recorded this event from the Kuiper Airborne Observatory, while other teams captured the event from various locations in Australia and New Zealand. Preceding this event, extensive astrometric observations of Pluto and the star were collected in order to refine the prediction.We will recount the investigations that led up to this important Pluto occultation, discuss the unexpected atmospheric results, and compare the 1988 event to the recent 2015 event whose shadow followed a similar track through New Zealand and Australia.

Modeling operational behavior of a disassembly line

NASA Astrophysics Data System (ADS)

Kizilkaya, Elif A.; Gupta, Surendra M.

2004-12-01

In this paper we present a dynamic kanban (pull) system specifically developed for disassembly lines. This type of kanban system is much more complex than the traditional kanban system used in assembly lines. For instance, unlike the assembly line where the external demand occurs only at the last station, the demands in the disassembly case also occur at any of the intermittent stations. The reason is that as a product moves on the disassembly line, various parts are disassembled at every station and accumulated at that station. Therefore, there are as many demand sources as there are number of parts. We consider a case example involving the end-of-life products. Based on the precedence relationships and other criteria such as hazardous properties of the parts, we balance the disassembly line. The results of the disassembly line-balancing problem (DLBP) are used as input to the proposed dynamic kanban system for disassembly line (DKSDL). We compare the performance of the DKSDL to the modified kanban system for disassembly line (MKSDL), which was previously introduced by the authors. We show, via simulation, that the DKSDL is far superior to MKSDL considered.

Radio Thermal Emission from Pluto and Charon during the New Horizons Encounter

NASA Astrophysics Data System (ADS)

Bird, Michael; Linscott, Ivan; Hinson, David; Tyler, G. L.; Strobel, Darrell F.; New Horizons Science Team

2017-10-01

As part of the New Horizons Radio-Science Experiment REX, radio thermal emission from Pluto and Charon (wavelength: 4.2 cm) was observed during the encounter on 14 July 2015. The primary REX measurement, a determination of the atmospheric height profile from the surface up to about 100 km, was conducted during an uplink radio occultation at both ingress and egress (Hinson et al., Icarus 290, 96-111, 2017). During the interval between ingress and egress, when the Earth and the REX uplink signals were occulted by the Pluto disk, the spacecraft antenna continued to point toward Earth and thus scanned diametrically across the Pluto nightside. The average diameter of the HGA 3 dB beam was ≈1100 km at the surface during this opportunity, thereby providing crudely resolved measurements of the radio brightness temperature across Pluto. The best resolution for the REX radiometry observations occurred shortly after closest approach, when the HGA was scanned twice across Pluto. These observations will be reported elsewhere (Linscott et al., Icarus, submitted, 2017). In addition to the resolved observations, full disk brightness temperature measurements of both bodies were performed during the approach (dayside) and departure (nightside) phases of the encounter. We present the results of these observations and provide a preliminary interpretation of the measured brightness temperatures.

Pluto and Charon in False Color Show Compositional Diversity

NASA Image and Video Library

2015-07-14

This July 13, 2015, image of Pluto and Charon is presented in false colors to make differences in surface material and features easy to see. It was obtained by the Ralph instrument on NASA's New Horizons spacecraft, using three filters to obtain color information, which is exaggerated in the image. These are not the actual colors of Pluto and Charon, and the apparent distance between the two bodies has been reduced for this side-by-side view. The image reveals that the bright heart-shaped region of Pluto includes areas that differ in color characteristics. The western lobe, shaped like an ice-cream cone, appears peach color in this image. A mottled area on the right (east) appears bluish. Even within Pluto's northern polar cap, in the upper part of the image, various shades of yellow-orange indicate subtle compositional differences. The surface of Charon is viewed using the same exaggerated color. The red on the dark northern polar cap of Charon is attributed to hydrocarbon materials including a class of chemical compounds called tholins. The mottled colors at lower latitudes point to the diversity of terrains on Charon. This image was taken at 3:38 a.m. EDT on July 13, one day before New Horizons' closest approach to Pluto. http://photojournal.jpl.nasa.gov/catalog/PIA19707

New Details on Pluto

NASA Image and Video Library

2015-07-10

This image of Pluto was taken by New Horizons' Long Range Reconnaissance Imager (LORRI) at 4:18 UT on July 9, 2015, from a range of 3.9 million miles (6.3 million kilometers). It reveals new details on the surface of Pluto, including complex patterns in the transition between the very dark equatorial band (nicknamed "the whale"), which occupies the lower part of the image, and the brighter northern terrain. The bright arc at the bottom of the disk shows that there is more bright terrain beyond the southern margin of the "whale." The side of Pluto that will be studied in great detail during the close encounter on July 14 is now rotating off the visible disk on the right hand side, and will not be seen again until shortly before closest approach. Three consecutive images were combined and sharpened, using a process called deconvolution, to create this view. Deconvolution enhances real detail but can also generate spurious features, including the bright edge seen on the upper and left margins of the disk (though the bright margin on the bottom of the disk is real). The wireframe globe shows the orientation of Pluto in the image: thicker lines indicate the equator and the prime meridian (the direction facing Charon). Central longitude on Pluto is 86°. http://photojournal.jpl.nasa.gov/catalog/PIA19705

The Surface Compositions of Triton, Pluto, and Charon

NASA Technical Reports Server (NTRS)

Cruikshank, Dale P.; Roush, Ted L.; Owen, Tobias C.; Quirico, Eric; DeBergh, Catherine

1995-01-01

Neptune's satellite Triton, and the planet-satellite binary Pluto and Charon, are the most distant planetary bodies on which ices have been directly detected. Triton and Pluto have very similar dimensions and mean densities, suggesting a similar or common origin. Through earth-based spectroscopic observations in the near-infrared, solid N2, CH4, and CO have been found on both bodies, with the additional molecule C02 on Triton. N2 dominates both surfaces, although the coverage is not spatially uniform. On Triton, the CH4 and CO are mostly or entirely frozen in the N2 matrix, while CO2 may be spatially segregated. On Pluto, some CH4 and the CO are frozen in the N2 matrix, but there is evidence for additional CH4 in a pure state, perhaps lying as a lag deposit on a subsurface layer of N2. Despite their compositional and dimensional similarities, Pluto and Triton are quite different from one another in detail. Additional hydrocarbons and other volatile ices have been sought spectroscopically but not yet have been detected. The only molecule identified on Pluto's satellite Charon is solid H2O, but the spectroscopic data are of low precision and admit the presence of other ices such as CH4.

Geology Before Pluto: Pre-encounter Considerations

NASA Astrophysics Data System (ADS)

Moore, J. M.

2014-12-01

Pluto, its large satellite Charon, and its four small known satellites represent the first trans-Neptunian Kuiper Belt objects populating the outer-most solar system beyond the gas giant planets to be studied in detail from a spacecraft (New Horizons). A complete picture of the solar nebula and solar system formation cannot be confidently formulated until representatives of this group of bodies at the edge of solar space have been examined. The Pluto system is composed of unique, lunar- and intermediate-sized objects that can tell us much about how objects with volatile icy compositions evolve. Modeling of the interior suggests that geologic activity may have been significant to some degree, and observations of frost on the surface could imply the need for a geologic reservoir for the replenishment of these phases. However, these putative indicators of Pluto's geologic history are inconclusive and unspecific. Detailed examination of Pluto's geologic record is the only plausible means of bridging the gap between theory and observation. In this talk I will examine the potential importance of these tentative indications of geologic activity and how specific spacecraft observations have been designed and used to constrain the Pluto system's geologic history. The cameras of New Horizons will provide robust data sets that should be immanently amenable to geological analysis of the Pluto system's landscapes. In this talk, we begin with a brief discussion of the planned observations by the New Horizons cameras that will bear most directly on geological interpretability. Then I will broadly review major geological processes that could potentially operate on the surfaces of Pluto and its moons. I will first survey exogenic processes (i.e., those for which energy for surface modification is supplied externally to the planetary surface): impact cratering, sedimentary processes (including volatile migration), and the work of wind. I will conclude with an assessment of the prospects for endogenic activity in the form of tectonics and cryovolcanism.

Tholins as Coloring Agents on Pluto and Other Icy Solar System Bodies

NASA Technical Reports Server (NTRS)

Cruikshank, Dale

2016-01-01

Tholins are refractory organic solids of complex structure and high molecular weight, with a wide range of color ranging from yellow and orange to dark red, and through tan to black. They are made in the laboratory by energy deposition (photons or charged particles) in gases and ices containing the simple molecules (e.g., N2, CH4, CO) found in planetary atmospheres or condensed on planetary surfaces. They are widely implicated in providing the colors and albedos, particularly in the region 0.3-1.0 microns, of several outer Solar System bodies, including Pluto, as well as aerosols in planetary atmospheres such as Titan. Recent color images of Pluto with the New Horizons spacecraft show concentrations of coloring agent(s) in some regions of the surface, and apparent near-absence in other regions. Tholins that may to some degree represent surface chemistry on Pluto have been synthesized in the laboratory by energetic processing of mixtures of the ices (N2, CH4, CO) known on Pluto's surface, or the same molecules in the gas phase. Details of the composition and yield vary with experimental conditions. Chemical analysis of Pluto ice tholins shows evidence of amides, carboxylic acids, urea, carbodiimides, and nitriles. Aromatic/olefinic, amide, and other functional groups are identified in XANES analysis. The ice tholins produced by e- irradiation have a higher concentration of N than UV ice tholins, with N/C approx. 0.9 (versus approx. 0.5 for UV tholins) and O/C approx.0.2. Raman spectra of the electron tholin show a high degree of structural disorder, while strong UV fluorescence indicates a large aromatic content. EUV photolysis of a Pluto gaseous atmosphere analog yields pale yellow solids relatively transparent in the visual, and with aliphatic CH bonds prominent in IR spectra. This or similar material may be responsible for Pluto's hazes.

Geology Before Pluto: Pre-encounter Considerations

NASA Astrophysics Data System (ADS)

Moore, Jeffrey

2014-05-01

Jeffrey M. Moore (NASA Ames) and the New Horizons Science Team Pluto, its large satellite Charon, and its four small known satellites represent the first trans-Neptunian Kuiper Belt objects populating the outer-most solar system beyond the gas giant planets to be studied in detail from a spacecraft (New Horizons). A complete picture of the solar nebula and solar system formation cannot be confidently formulated until representatives of this group of bodies at the edge of solar space have been examined. The Pluto system is composed of unique, lunar- and intermediate-sized objects that can tell us much about how objects with volatile icy compositions evolve. Modeling of the interior suggests that geologic activity may have been significant to some degree, and observations of frost on the surface could imply the need for a geologic reservoir for the replenishment of these phases. However, these putative indicators of Pluto's geologic history are inconclusive and unspecific. Detailed examination of Pluto's geologic record is the only plausible means of bridging the gap between theory and observation. In this talk I will examine the potential importance of these tentative indications of geologic activity and how specific spacecraft observations have been designed and used to constrain the Pluto system's geologic history. The cameras of New Horizons will provide robust data sets that should be immanently amenable to geological analysis of the Pluto System's landscapes. In this talk, we begin with a brief discussion of the planned observations by the New Horizons cameras that will bear most directly on geological interpretability. Then I will broadly review major geological processes that could potentially operate on the surfaces of Pluto and its moons. I will first survey exogenic processes (i.e. those for which energy for surface modification is supplied externally to the planetary surface): impact cratering, sedimentary processes (including volatile migration), and the work of wind. I will conclude with an assessment of the prospects for endogenic activity in the form of tectonics and cryo-volcanism.

Geology Before Pluto: Pre-Encounter Considerations

NASA Technical Reports Server (NTRS)

Moore, Jeffrey M.

2014-01-01

Pluto, its large satellite Charon, and its four known satellites represent the first trans-Neptunian Kuiper Belt objects populating the outer-most solar system beyond the gas giant planets to be studied in detail from a spacecraft (New Horizons). A complete picture of the solar nebula, and solar system formation cannot be confidently formulated until representatives of this group of bodies at the edge of solar space have been examined. The Pluto system is composed of unique lunar- and intermediate-sized objects that can tell us much about how objects with volatile icy compositions evolve. Modeling of the interior suggests that geologic activity may have been to some degree, and observations of frost on the surface could imply the need for a geologic reservoir for the replenishment of these phases. However, the putative indicators of Pluto's geologic history are inconclusive and unspecific. Detailed examination of Pluto's geologic record is the only plausible means of bridging the gap between theory and observations. In this talk I will examine the potential importance of these tentative indications of geologic activity and how specific spacecraft observations have been designed and used to constrain the Pluto system's geologic history. The cameras of New Horizons will provide robust data sets that should be immanently amenable to geological analysis of the Pluto System's landscapes. In this talk, we begin with a brief discussion of the planned observations by New Horizons' cameras that will bear most directly on geological interpretability. Then I will broadly review major geological processes that could potentially operate of the surfaces of Pluto and its moons. I will first survey exogenic processes (i.e., those for which energy for surface modification is supplied externally to the planetary surface): impact cratering, sedimentary processes (including volatile migration) and the work of wind. I will conclude with an assessment of prospects for endogenic activity in the form of tectonics and cryo-volcanism.

New Horizons Results at Charon

NASA Astrophysics Data System (ADS)

Buratti, B. J.; Stern, A.; Moore, J. M.; Weaver, H. A., Jr.; Grundy, W. M.; Hofgartner, J. D.; Spencer, J. R.; McKinnon, W. B.; Olkin, C.; Young, L. A.; Verbiscer, A.; Singer, K. N.; Robbins, S. J.; Ennico Smith, K.

2016-12-01

The New Horizons Spacecraft encountered dwarf planet Pluto and its system of moons on July 15, 2015 for the first detailed study of a Kuiper Belt Object (1). Pluto possesses a system of at least 5 moons, including Charon, which is the largest moon in relation to its primary, comprising 12% of the mass of Pluto. The results from the flyby show a world that has undergone a large resurfacing event on at least one of its hemispheres, perhaps from differentiation and subsequent freezing of a subsurface ocean. Charon has a complex system of faults, and regions of various ages based on crater counting statistics. It has no evidence for recent or ongoing geologic activity as Pluto does. Its visible geometric albedo is 0.41±0.02, with normal reflectances ranging from 0.2-0.7. A few isolated brighter areas exist. A northern polar cap of low-albedo red material may be formed from a newly discovered process in the Solar System: the capture of methane from Pluto's atmosphere and subsequent polymerization and accumulation of a complex lag deposit (2). Unlike Pluto, which has a surface covered primarily of methane and nitrogen, Charon's surface is composed of water ice, along with NH3-ice in some form (3). The substantial relief on the moon implies that ice extends below the surface. The bulk density of Pluto and Charon are similar (1). This result implies that if Charon was formed from an impact and reaccretion event involving Pluto and a second body (4), it is unlikely the two bodies were fully differentiated prior to the event. (1) Stern, S. A. et al. (2015). Science 350, 292. (2) Grundy, W. M. et al. (2016). Manuscript accepted at Nature. (3) Grundy, W. M. et al. (2016). Science 351, 1283. (4) Canup, R. M. (2011). Astron. J. 141, 35. Funded by NASA.

Ground-based Light Curves Two Pluto Days Before the New Horizons Passage

NASA Astrophysics Data System (ADS)

Bosh, A. S.; Pasachoff, J. M.; Babcock, B. A.; Durst, R. F.; Seeger, C. H.; Levine, S. E.; Abe, F.; Suzuki, D.; Nagakane, M.; Sickafoose, A. A.; Person, M. J.; Zuluaga, C.; Kosiarek, M. R.

2015-12-01

We observed the occultation of a 12th magnitude star, one of the two brightest occultation stars ever in our dozen years of continual monitoring of Pluto's atmosphere through such studies, on 29 June 2015 UTC. At Canterbury University's Mt. John University Observatory on the south island of New Zealand, in clear sky, we used our POETS frame-transfer CCD at 10 Hz with GPS timing on the 1-m McLellan telescope as well as an infrared camera on an 0.6-m telescope and three-color photometry at a slower cadence on a second 0.6-m telescope. The light curves show a central flash, indicating that we were close to the center of the occultation path, and allowing us to explore Pluto's atmosphere lower than usual. The light curves show that Pluto's atmosphere remained robust. Observations from 0.5- and 0.4-m telescopes at the Auckland Observatory gave the first half of the occultation before clouds came in. We coordinated our observations with aircraft observations with NASA's Stratospheric Observatory for Infrared Astronomy (SOFIA) and its High Speed Imaging Photometer for Occultations (HIPO). Our ground-based and airborne stellar-occultation effort came only just over two weeks of Earth days and two Pluto days (based on Pluto's rotational period) before the flyby of NASA's New Horizons spacecraft, meaning that the mission's exquisite snapshot of Pluto's atmosphere can be placed in the context of our series of ground-based occultation observations carried out on a regular basis since 2002 following a first Pluto occultation observed in 1988 from aloft. Our observations were supported by NASA Planetary Astronomy grants NNX12AJ29G to Williams College, NNX15AJ82G to Lowell Observatory, and NNX10AB27G to MIT, and by the National Research Foundation of South Africa. We thank Alan Gilmore, Pam Kilmartin, Robert Lucas, Paul Tristam, and Carolle Varughese for assistance at Mt. John.

Observational Constraints on a Pluto Torus of Circumsolar Neutral Gas

NASA Astrophysics Data System (ADS)

Hill, M. E.; Kollmann, P.; McNutt, R. L., Jr.; Smith, H. T.; Bagenal, F.; Brown, L. E.; Elliott, H. A.; Haggerty, D. K.; Horanyi, M.; Krimigis, S. M.; Kusterer, M. B.; Lisse, C. M.; McComas, D. J.; Piquette, M. R.; Sidrow, E. J.; Strobel, D. F.; Szalay, J.; Vandegriff, J. D.; Zirnstein, E.; Ennico Smith, K.; Olkin, C.; Weaver, H. A., Jr.; Young, L. A.; Stern, S. A.

2015-12-01

We present the concept of a neutral gas torus surrounding the Sun, aligned with Pluto's orbit, and place observational constraints based primarily on comparison of New Horizons (NH) measurements with a 3-D Monte Carlo model adapted from analogous satellite tori surrounding Saturn and Jupiter. Such a torus, or perhaps partial torus, should result from neutral N2 escaping from Pluto's exosphere. Unlike other more massive planets closer to the Sun, neutrals escape Pluto readily owing, e.g., to the high thermal speed relative to the escape velocity. Importantly, escaped neutrals have a long lifetime due to the great distance from the Sun, ~100 years for photoionization of N2 and ~180 years for photoionization of N, which results from disassociated N2. Despite the lengthy 248-year orbit, these long e-folding lifetimes may allow an enhanced neutral population to form an extended gas cloud that modifies the N2 spatial profile near Pluto. These neutrals are not directly observable by NH but once ionized N2+ or N+ are picked up by the solar wind, reaching ~50 keV, making these pickup ions (PUIs) detectable by NH's Pluto Energetic Particle Spectrometer Science Investigation (PEPSSI) instrument. PEPSSI observations analyzed to date may constrain the N2 density; the remaining ~95% of the encounter data, scheduled for downlink in August along with similarly anticipated data from the Solar Wind Around Pluto (SWAP) experiment, should help determine the Pluto outgassing rates. Measurements from SWAP include the solar wind speed, a quantity that greatly enhances PUI studies by enabling us to directly account for the PUI distribution's sensitive dependence on plasma speed. Note that anomalous cosmic ray Si observed at Voyager is overabundant by a factor of ~3000 relative to interstellar composition. This might be related to "outer source" PUIs, but the fact that N2 and Si are indistinguishable in many instruments could mean that N2 is actually driving this apparent Si discrepancy.

Ground and space-based separate PSF photometry of Pluto and Charon from New Horizons and Magellan

NASA Astrophysics Data System (ADS)

Zangari, Amanda M.; Stern, S. A.; Young, L. A.; Weaver, H. A.; Olkin, C.; Buratti, B. J.; Spencer, J.; Ennico, K.

2013-10-01

While Pluto and Charon are easily resolvable in some space-based telescopes, ground-based imaging of Pluto and Charon can yield separate PSF photometry in excellent seeing. We present B and Sloan g', r', i', and z' separate photometry of Pluto and Charon taken at the Magellan Clay telescope using LDSS-3. In 2011, observations were made on 7, 8, 9, 19, and 20 March, at 9:00 UT, covering sub-Earth longitudes 130°, 74°, 17°, 175° and 118°. The solar phase angle ranged from 1.66-1.68° to 1.76-1.77°. In 2012, observations were made on February 28, 29 and March 1 at 9:00 UT covering longitudes 342°, 110° and 53° and on May 30 and 31 at 9:30 UT and 7:00 UT, covering longitudes 358° and 272°. Solar phase angles were 1.53-1.56° and 0.89°-0.90° degrees. All longitudes use the convention of zero at the sub-Charon longitude and decrease in time. Seeing ranged from 0.46 to 1.26 arcsecond. We find that the mean rotationally-averaged Charon-to-Pluto light ratio is 0.142±0.003 for Sloan r',i' and z'. Charon is brighter in B and g', with a light ratio of 0.182±0.003 and 0.178±0.002 respectively. Additionally, we present separate PSF photometry of Pluto and Charon from New Horizons images taken by the LORRI instrument on 1 and 3 July 2013 at 17:00 UT and 23:00 UT, sub-Earth longitude 251° and 125°. We find that the rotation-dependent variations in the light ratio are consistent with earlier estimates such as those from Buie et al. 2010, AJ 139, 1117-1127. However, at a solar phase angle of 10.9°, Charon appears 0.25 magnitudes fainter relative to Pluto at the same rotational phase than measurements from the ground with the largest possible solar phase angle. Thus we provide the first estimate of a Pluto phase curve beyond 2°. These results represent some of the first Pluto science from New Horizons. This work has been funded in part by NASA Planetary Astronomy Grant NNX10AB27G and NSF Award 0707609 to MIT and by NASA's New Horizons mission to Pluto.

Final postflight hardware evaluation report RSRM-28 (STS-53)

NASA Technical Reports Server (NTRS)

Starrett, William David, Jr.

1993-01-01

The final report for the Clearfield disassembly evaluation and a continuation of the KSC postflight assessment for the RSRM-28 (STS-53) RSRM flight set is presented. All observed hardware conditions were documented on PFOR's and are included in Appendices A through C. Appendices D and E contain the measurements and safety factor data for the nozzle and insulation components. This report, along with the KSC Ten-Day Postflight Hardware Evaluation Report (TWR-64215), represents a summary of the RSRM-28 hardware evaluation. The as-flown hardware configuration is documented in TWR-63638. Disassembly evaluation photograph numbers are logged in TWA-1989. The RSRM-28 flight set disassembly evaluations described were performed at the RSRM Refurbishment Facility in Clearfield, Utah. The final factory joint demate occurred on July 15, 1993. Additional time was required to perform the evaluation of the stiffener rings per special issue 4.1.5.2 because of the washout schedule. The release of this report was after completion of all special issues per program management direction. Detailed evaluations were performed in accordance with the Clearfield PEEP, TWR-50051, Revision A. All observations were compared against limits that are also defined in the PEEP. These limits outline the criteria for categorizing the observations as acceptable, reportable, or critical. Hardware conditions that were unexpected and/or determined to be reportable or critical were evaluated by the applicable team and tracked through the PFAR system.

40. INTERIOR VIEW TO THE SOUTHEAST OF ROOM 302, A ...

Library of Congress Historic Buildings Survey, Historic Engineering Record, Historic Landscapes Survey

40. INTERIOR VIEW TO THE SOUTHEAST OF ROOM 302, A SMALL ISOLATED OFFICE ON THE THIRD FLOOR ON THE EAST SIDE OF THE DISASSEMBLY BAY. A METAL SPIRAL STAIRCASE IS IN THE SOUTHEAST CORNER AND HATCHWAYS ARE IN THE CEILING AND FLOOR TOWARD THE EAST SIDE OF THE ROOM. - Nevada Test Site, Reactor Maintenance Assembly & Dissassembly Facility, Area 25, Jackass Flats, Junction of Roads F & G, Mercury, Nye County, NV

Informal Names for Features on Pluto Moon Charon

NASA Image and Video Library

2015-07-29

This image contains the initial, informal names being used by NASA's New Horizons team for the features on Pluto's largest moon, Charon. Names were selected based on the input the team received from the Our Pluto naming campaign. Names have not yet been approved by the International Astronomical Union (IAU). For more information on the maps and feature naming, visit http://www.ourpluto.org/maps. http://photojournal.jpl.nasa.gov/catalog/PIA19864

Informal Names for Features on Pluto Sputnik Planum

NASA Image and Video Library

2015-07-29

This image contains the initial, informal names being used by NASA's New Horizons team for the features on Pluto's Sputnik Planum (plain). Names were selected based on the input the team received from the Our Pluto naming campaign. Names have not yet been approved by the International Astronomical Union (IAU). For more information on the maps and feature naming, visit http://www.ourpluto.org/maps. http://photojournal.jpl.nasa.gov/catalog/PIA19865

Informal Names for Features on Pluto

NASA Image and Video Library

2015-07-29

This image contains the initial, informal names being used by NASA's New Horizons team for the features and regions on the surface of Pluto. Names were selected based on the input the team received from the Our Pluto naming campaign. Names have not yet been approved by the International Astronomical Union (IAU). For more information on the maps and feature naming, visit http://www.ourpluto.org/maps. http://photojournal.jpl.nasa.gov/catalog/PIA19863

Compiler-Driven Performance Optimization and Tuning for Multicore Architectures

DTIC Science & Technology

2015-04-10

develop a powerful system for auto-tuning of library routines and compute-intensive kernels, driven by the Pluto system for multicores that we are...kernels, driven by the Pluto system for multicores that we are developing. The work here is motivated by recent advances in two major areas of...automatic C-to-CUDA code generator using a polyhedral compiler transformation framework. We have used and adapted PLUTO (our state-of-the-art tool

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Fran Bagenal, senior scientist at the University of Colorado, speaks during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Alan Stern, Principal Investigator on NASA's New Horizons Mission, delivers closing remarks following a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Fran Bagenal, senior scientist at the University of Colorado, far right, speaks during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Bonnie Buratti, senior scientist at NASA's Jet Propultion Laboratory, speaks during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

Low cytoplasmic pH reduces ER-Golgi trafficking and induces disassembly of the Golgi apparatus

DOE Office of Scientific and Technical Information (OSTI.GOV)

Soonthornsit, Jeerawat; Yamaguchi, Yoko; Tamura, Daisuke

The Golgi apparatus was dramatically disassembled when cells were incubated in a low pH medium. The cis-Golgi disassembled quickly, extended tubules and spread to the periphery of cells within 30 min. In contrast, medial- and trans-Golgi were fragmented in significantly larger structures of smaller numbers at a slower rate and remained largely in structures distinct from the cis-Golgi. Electron microscopy revealed the complete disassembly of the Golgi stack in low pH treated cells. The effect of low pH was reversible; the Golgi apparatus reassembled to form a normal ribbon-like structure within 1–2 h after the addition of a control medium.more » The anterograde ER to Golgi transport and retrograde Golgi to ER transport were both reduced under low pH. Phospholipase A{sub 2} inhibitors (ONO, BEL) effectively suppressed the Golgi disassembly, suggesting that the phospholipase A{sub 2} was involved in the Golgi disassembly. Over-expression of Rab1, 2, 30, 33 and 41 also suppressed the Golgi disassembly under low pH, suggesting that they have protective role against Golgi disassembly. Low pH treatment reduced cytoplasmic pH, but not the luminal pH of the Golgi apparatus, strongly suggesting that reduction of the cytoplasmic pH triggered the Golgi disassembly. Because a lower cytoplasmic pH is induced in physiological or pathological conditions, disassembly of the Golgi apparatus and reduction of vesicular transport through the Golgi apparatus may play important roles in cell physiology and pathology. Furthermore, our findings indicated that low pH treatment can serve as an important tool to analyze the molecular mechanisms that support the structure and function of the Golgi apparatus. - Highlights: • The Golgi apparatus reversibly disassembles by low pH treatment. • The cis-Golgi disassembles quickly generating tubular structures. • Both anterograde and retrograde transport between the ER and the Golgi apparatus are reduced. • Phospholipase A{sub 2} inhibitors (ONO-RS082, BEL) prevented the low pH induced Golgi disassembly. • Rab1, 2, 30, 33 and 41 suppress low pH induced Golgi disassembly.« less

The visible spectrum of Pluto: secular and longitudinal variation

NASA Astrophysics Data System (ADS)

Lorenzi, Vania; Pinilla-Alonso, Noemí; Emery, Joshua P.; Licandro, Javier; Cruikshank, Dale P.; Grundy, Will; Binzel, Richard P.

2015-11-01

Continuous near-infrared spectroscopic observations during the last 30 years enabled the characterization of the Pluto's surface and the study of its variability. Nevertheless, only few data are available in the visible range, where the nature of the complex-organics can be studied.For this reason, we started an observational campaign to obtain the Pluto's relative reflectance in the visible range, with the aim of characterizing the different components of its surface, and providing ground based observations in support of the New Horizons mission. We observed Pluto on six nights in 2014, with the imager/spectrograph ACAM@WHT (La Palma, Spain). We obtained six spectra in the 0.40 - 0.93 µm range, that covered a whole Pluto's rotational period (6.4 days).To study longitudinal variations, we computed for all the spectra the spectral slope, and the position and the depth of the methane ice absorption bands. Also, to search for secular or seasonal variations we compared our data with previously published results.All the spectra present a red slope, indicating the presence of complex organics on Pluto's surface, and show the methane ice absorption bands between 0.73 and 0.90 μm. We also report the detection of the CH4 absorption band at 0.62 μm, already detected in the spectra of Makemake and Eris. The measurement of the band depth at 0.62 μm in the new spectra of Pluto, and in the spectra of Makemake and Eris, permits us to estimate the Lambert coefficient, not measured yet at this wavelength, at a temperature of 30 K and 40 K.We find that all the CH4 bands present a blue shift. This shift is minimum at the Charon-facing hemisphere, where the CH4 is also more abundant, indicating a higher degree of saturation of CH4 in the CH4:N2 dilution at this hemisphere.Comparing with data in the literature, we found that the longitudinal and secular variations of the parameters measured in our spectra are in accordance with previous results and with the distribution of the dark and bright material as showed by the Pluto's albedo maps from New Horizons.In 2015, new observations were run quasi-simultaneously with the New Horizons flyby at 10 different Pluto longitudes (July 3 to 14) . The data are currently being reduced.

Rarefied gas dynamic simulation of transfer and escape in the Pluto-Charon system

NASA Astrophysics Data System (ADS)

Hoey, William A.; Yeoh, Seng Keat; Trafton, Laurence M.; Goldstein, David B.; Varghese, Philip L.

2017-05-01

We apply the direct simulation Monte Carlo rarefied gas dynamic technique to simulations of Pluto's rarefied upper atmosphere motivated by the need to better understand New Horizons (NH) data. We present a novel three-dimensional DSMC model of the atmosphere that spans from several hundred km below the exobase - where continuum flow transitions to the rarefied regime - to fully free-molecular flow hundreds of thousands of km from Pluto's center. We find molecular collisions in Pluto's upper atmosphere to be significant in shaping the flowfield, both by promoting flux from the plutonian exobase to Charon and by increasing the proportion of that flux generated on the exobase's anti-Charon hemisphere. Our model accounts for the gravitational fields of both Pluto and Charon, the centripetal and Coriolis forces due to the rotation of Pluto in our reference frame, and the presence of Charon as a temporary sink for impacting particles. Using this model, we analyze the escape processes of N2 and CH4 from Pluto across different solar heating conditions, and evaluate the three-dimensional structure of the upper plutonian atmosphere, including gas transfer to and deposition on Charon. We find results consistent with the NH-determined escape rate, upper atmospheric temperature, and lack of a detectable Charon atmosphere. Gas-transfer structures are noted in a binary atmospheric configuration, including preferential deposition of material from Pluto's escaping atmosphere onto Charon's leading hemisphere that peaks at 315° E on the equator. As the moon gravitationally focuses incident flow, a high density structure forms in its wake. If molecules are permitted to escape from Charon in diffuse reflections from its surface, a returning flux forms to Pluto's exobase, preferentially directed toward its trailing hemisphere. Charon is capable of supporting a thin atmosphere at column densities as high as 1.5 × 1017 m-2 in simulations with a plutonian exobase condition similar to the NH encounter. Results computed from a fit to the NH encounter exobase (Gladstone et al., 2016) predict a system escape rate of 7 × 1025 CH4 s-1 in close agreement with those reported by NH (Bagenal et al., 2016; Gladstone et al., 2016), and a net depositional flux to Charon of 2 × 1024 s-1, of which ∼98% is methane.

29 CFR 1926.1403 - Assembly/Disassembly-selection of manufacturer or employer procedures.

Code of Federal Regulations, 2013 CFR

2013-07-01

... 29 Labor 8 2013-07-01 2013-07-01 false Assembly/Disassembly-selection of manufacturer or employer... CONSTRUCTION Cranes and Derricks in Construction § 1926.1403 Assembly/Disassembly—selection of manufacturer or... applicable to assembly and disassembly, or (b) Employer procedures for assembly and disassembly. Employer...

29 CFR 1926.1403 - Assembly/Disassembly-selection of manufacturer or employer procedures.

Code of Federal Regulations, 2012 CFR

2012-07-01

... 29 Labor 8 2012-07-01 2012-07-01 false Assembly/Disassembly-selection of manufacturer or employer... CONSTRUCTION Cranes and Derricks in Construction § 1926.1403 Assembly/Disassembly—selection of manufacturer or... applicable to assembly and disassembly, or (b) Employer procedures for assembly and disassembly. Employer...

29 CFR 1926.1403 - Assembly/Disassembly-selection of manufacturer or employer procedures.

Code of Federal Regulations, 2014 CFR

2014-07-01

... 29 Labor 8 2014-07-01 2014-07-01 false Assembly/Disassembly-selection of manufacturer or employer... CONSTRUCTION Cranes and Derricks in Construction § 1926.1403 Assembly/Disassembly—selection of manufacturer or... applicable to assembly and disassembly, or (b) Employer procedures for assembly and disassembly. Employer...

29 CFR 1926.1403 - Assembly/Disassembly-selection of manufacturer or employer procedures.

Code of Federal Regulations, 2011 CFR

2011-07-01

... 29 Labor 8 2011-07-01 2011-07-01 false Assembly/Disassembly-selection of manufacturer or employer... CONSTRUCTION Cranes and Derricks in Construction § 1926.1403 Assembly/Disassembly—selection of manufacturer or... applicable to assembly and disassembly, or (b) Employer procedures for assembly and disassembly. Employer...

Resolved, Time-Series Observations of Pluto-Charon with the Magellan Telescopes

NASA Astrophysics Data System (ADS)

Elliot, J. L.; Person, M. J.; Adams, E. R.; Gulbis, A. A. S.; Kramer, E. A.

2005-08-01

In support of prediction refinements at MIT for stellar occultations by Pluto and Charon, resolved photometric observations of Pluto and Charon at optical wavelengths have been carried out with the Magellan telescopes at Las Campanas Observatory for each apparition since 2001. Both Sloan and Johnson-Kron-Cousins filters have been used. The median natural image quality for the site is about 0.7 arcsec (with some nights better than 0.3 arcsec). These data yield accurate light ratios for the two bodies as a function of: (1) wavelength, (2) Charon's orbital phase, and (3) the sub-Earth latitude for Pluto and Charon. This information is needed to interpret the location of their center of light, relative to their center of mass, for unresolved images of Pluto and Charon taken with wide-field astrometric instruments. The Raymond and Beverly Magellan Instant Camera ("MagIC") -- the instrument used for these observations -- has a focal-plane scale of 0.069 arcsec/pix and a field of 2.3 arcmin. This field is large enough so that many of our Pluto-Charon frames can be tied to the International Coordinate Reference Frame (ICRF) with stars in the UCAC2 catalog. Initial results for this program have been reported by Clancy et al. (Highlights of Astr. vol. 13, in press), who found a strong trend in the Charon to Pluto light ratio over the wavelength range spanned by the Sloan filters. Further results from this program used to predict the 2005 July 11 stellar occultation by Charon will be presented. We gratefully acknowledge support from NASA Grant NNG04GF25G from the Planetary Astronomy program.

Investigating the present and past glacial and frost activity on Pluto with a volatile transport model

NASA Astrophysics Data System (ADS)

Bertrand, Tanguy; Forget, Francois

2016-10-01

The high obliquity and eccentricity of the orbit of Pluto induce seasonal cycles of condensation and sublimation of the main volatile ices: N2, CH4, and CO. The New Horizons spacecraft, which flew by Pluto in July 2015, revealed a complex surface composition including a thousand-kilometre nitrogen glacier in the "Sputnik Planum" plain near the Anti-Charon longitude, extensive methane frosts at mid and high latitudes, and equatorial ice-free regions. We present numerical simulations designed to model the evolution of Pluto's volatiles over thousands of years on the basis of straightforward universal physical equations.Our results explain the observed distribution of ices on the surface and the quantities of volatiles in the atmosphere. In particular the model predicts the N2 ice accumulation in the deepest low-latitude basin and the 3-fold increase of pressure observed to occur since 1988. This points to atmospheric-topographic processes at the origin of the Sputnik Planum's nitrogen glacier. The same simulations also show frosts of methane, and sometimes nitrogen, that seasonally cover the mid and high latitudes, explaining the bright northern polar cap reported in the 1990s and the observed ice distribution in 2015. The model also predicts that most of these seasonal frosts should disappear in the next decade, and thus could be tested observationally in the near future.Using prior orbital parameters of Pluto and a realistic glacial flow parametrization, we also simulate past climates of Pluto. The results show that Pluto undergoes cycles of glacial activity (over timescales of few million years) that may explain the rugged eroded-mountain landscapes surrounding Sputnik Planum and the "bladed" methane terrains east of "Tombaugh Regio".

Craters of the Pluto-Charon system

NASA Astrophysics Data System (ADS)

Robbins, Stuart J.; Singer, Kelsi N.; Bray, Veronica J.; Schenk, Paul; Lauer, Tod R.; Weaver, Harold A.; Runyon, Kirby; McKinnon, William B.; Beyer, Ross A.; Porter, Simon; White, Oliver L.; Hofgartner, Jason D.; Zangari, Amanda M.; Moore, Jeffrey M.; Young, Leslie A.; Spencer, John R.; Binzel, Richard P.; Buie, Marc W.; Buratti, Bonnie J.; Cheng, Andrew F.; Grundy, William M.; Linscott, Ivan R.; Reitsema, Harold J.; Reuter, Dennis C.; Showalter, Mark R.; Tyler, G. Len; Olkin, Catherine B.; Ennico, Kimberly S.; Stern, S. Alan; New Horizons Lorri, Mvic Instrument Teams

2017-05-01

NASA's New Horizons flyby mission of the Pluto-Charon binary system and its four moons provided humanity with its first spacecraft-based look at a large Kuiper Belt Object beyond Triton. Excluding this system, multiple Kuiper Belt Objects (KBOs) have been observed for only 20 years from Earth, and the KBO size distribution is unconstrained except among the largest objects. Because small KBOs will remain beyond the capabilities of ground-based observatories for the foreseeable future, one of the best ways to constrain the small KBO population is to examine the craters they have made on the Pluto-Charon system. The first step to understanding the crater population is to map it. In this work, we describe the steps undertaken to produce a robust crater database of impact features on Pluto, Charon, and their two largest moons, Nix and Hydra. These include an examination of different types of images and image processing, and we present an analysis of variability among the crater mapping team, where crater diameters were found to average ± 10% uncertainty across all sizes measured (∼0.5-300 km). We also present a few basic analyses of the crater databases, finding that Pluto's craters' differential size-frequency distribution across the encounter hemisphere has a power-law slope of approximately -3.1 ± 0.1 over diameters D ≈ 15-200 km, and Charon's has a slope of -3.0 ± 0.2 over diameters D ≈ 10-120 km; it is significantly shallower on both bodies at smaller diameters. We also better quantify evidence of resurfacing evidenced by Pluto's craters in contrast with Charon's. With this work, we are also releasing our database of potential and probable impact craters: 5287 on Pluto, 2287 on Charon, 35 on Nix, and 6 on Hydra.

New Horizons Alice sky Lyman-α at Pluto encounter: Importance for photochemistry

NASA Astrophysics Data System (ADS)

Retherford, K. D.; Gladstone, R.; Stern, S. A.; Weaver, H. A., Jr.; Young, L. A.; Olkin, C.; Cheng, A. F.; Greathouse, T.; Kammer, J.; Linscott, I.; Parker, A. H.; Parker, J. W.; Schindhelm, E.; Singer, K. N.; Steffl, A.; Strobel, D. F.; Summers, M. E.; Tsang, C.; Tyler, G. L.; Versteeg, M.; Woods, W. W.; Ennico Smith, K.; Hinson, D. P.; Pryor, W. R.; Cunningham, N. J.; Curdt, W.

2015-12-01

The third zone of our solar system, including the Pluto system, has a unique illumination environment at UV wavelengths. While direct solar Lyman-α emissions dominate the signal at 121.6 nm at classical solar system distances, the contribution of illumination by Interplanetary Medium (IPM) Lyman-α sky-glow is roughly on par at Pluto (Gladstone et al. 2015). The Pluto-Alice UV imaging spectrograph on New Horizons conducted several dedicated sky scans to measure the IPM Lyman-α both en route to and while at Pluto. These scans provide 6° by 360° great-circle swaths while spinning the spacecraft. Three sets of scans conducted en route are reported in Gladstone et al. (2012). During the Pluto encounter, sets of scans with six such swaths evenly spaced ~30° apart for all-sky coverage were obtained just before closest approach and again just after. These measurements agree well with brightness variations expected for IPM brightnesses peaking in the sunward direction and interspersed with detections of UV bright stars and other sky features. Previous studies estimated contributions of ~2/3rds direct solar Lyα and 1/3rd IPM Lyα. Our early results suggest that these model predictions need revision. These findings have important implications for determining the rates of photochemical reactions within Pluto's atmosphere that are driven by UV photons at 121.6 nm. Similarly, new constraints are provided to the rates of photolysis on Charon's polar winter nightside. These constraints are useful for understanding the volatile transport and long-term stability of the dark red region near Charon's pole discovered by New Horizons.

METHANE AND NITROGEN ABUNDANCES ON PLUTO AND ERIS

DOE Office of Scientific and Technical Information (OSTI.GOV)

Tegler, S. C.; Cornelison, D. M.; Abernathy, M. R.

We present spectra of Eris from the MMT 6.5 m Telescope and Red Channel Spectrograph (5700-9800 A, 5 A pixel{sup -1}) on Mt. Hopkins, AZ, and of Pluto from the Steward Observatory 2.3 m Telescope and Boller and Chivens Spectrograph (7100-9400 A, 2 A pixel{sup -1}) on Kitt Peak, AZ. In addition, we present laboratory transmission spectra of methane-nitrogen and methane-argon ice mixtures. By anchoring our analysis in methane and nitrogen solubilities in one another as expressed in the phase diagram of Prokhvatilov and Yantsevich, and comparing methane bands in our Eris and Pluto spectra and methane bands in ourmore » laboratory spectra of methane and nitrogen ice mixtures, we find Eris' bulk methane and nitrogen abundances are {approx}10% and {approx}90% and Pluto's bulk methane and nitrogen abundances are {approx}3% and {approx}97%. Such abundances for Pluto are consistent with values reported in the literature. It appears that the bulk volatile composition of Eris is similar to the bulk volatile composition of Pluto. Both objects appear to be dominated by nitrogen ice. Our analysis also suggests, unlike previous work reported in the literature, that the methane and nitrogen stoichiometry is constant with depth into the surface of Eris. Finally, we point out that our Eris spectrum is also consistent with a laboratory ice mixture consisting of 40% methane and 60% argon. Although we cannot rule out an argon-rich surface, it seems more likely that nitrogen is the dominant species on Eris because the nitrogen ice 2.15 {mu}m band is seen in spectra of Pluto and Triton.« less

Long-term surface temperature modeling of Pluto

NASA Astrophysics Data System (ADS)

Earle, Alissa M.; Binzel, Richard P.; Young, Leslie A.; Stern, S. A.; Ennico, K.; Grundy, W.; Olkin, C. B.; Weaver, H. A.; New Horizons Geology and Geophysics Imaging Team

2017-05-01

NASA's New Horizons' reconnaissance of the Pluto system has revealed at high resolution the striking albedo contrasts from polar to equatorial latitudes on Pluto, as well as the sharpness of boundaries for longitudinal variations. These contrasts suggest that Pluto must undergo dynamic evolution that drives the redistribution of volatiles. Using the New Horizons results as a template, we explore the surface temperature variations driven seasonally on Pluto considering multiple timescales. These timescales include the current orbit (248 years) as well as the timescales for obliquity precession (peak-to-peak amplitude of 23° over 3 million years) and regression of the orbital longitude of perihelion (3.7 million years). These orbital variations create epochs of ;Extreme Seasons; where one pole receives a short, relatively warm summer and long winter, while the other receives a much longer, but less intense summer and short winter. We use thermal modeling to build upon the long-term insolation history model described by Earle and Binzel (2015) and investigate how these seasons couple with Pluto's albedo contrasts to create temperature effects. From this study we find that a bright region at the equator, once established, can become a site for net deposition. We see the region informally known as Sputnik Planitia as an example of this, and find it will be able to perpetuate itself as an ;always available; cold trap, thus having the potential to survive on million year or substantially longer timescales. Meanwhile darker, low-albedo, regions near the equator will remain relative warm and generally not attract volatile deposition. We argue that the equatorial region is a ;preservation zone; for whatever albedo is seeded there. This offers insight as to why the equatorial band of Pluto displays the planet's greatest albedo contrasts.

Pluto's Haze from 2002 - 2015: Correlation with the Solar Cycle

NASA Astrophysics Data System (ADS)

Young, Eliot; Klein, Viliam; Hartig, Kara; Resnick, Aaron; Mackie, Jason; Carriazo, Carolina; Watson, Charles; Skrutskie, Michael; Verbiscer, Anne; Nelson, Matthew; Howell, Robert; Wasserman, Lawrence; Hudson, Gordon; Gault, David; Barry, Tony; Sicardy, Bruno; Cole, Andrew; Giles, Barry; Hill, Kym

2017-04-01

Occultations by Pluto were observed 2002, 2007, 2011 and 2015, with each event observed simultaneously in two or more wavelengths. Separate wavelengths allow us to discriminate between haze opacity and refractive effects due to an atmosphere's thermal profile - these two effects are notoriously hard to separate if only single-wavelength lightcurves are available. Of those four occultations, the amount of haze in Pluto's atmosphere was highest in 2002 (Elliot et al. 2003 report an optical depth of 0.11 at 0.73 µm in the zenith direction), but undetectable in the 2007 and 2011 events (we find optical depth upper limits of 0.012 and 0.010 at 0.6 µm). Cheng et al. (2016) report a zenith optical depth of 0.018 at 0.6 µm from the haze profiles seen in New Horizons images. These four data points are correlated with the solar cycle. The 2002 haze detection occurred just after the peak of solar cycle 23, the 2007 and 2011 non-detections occurred during the solar minimum between peaks 23 and 24, and the New Horizons flyby took place just after the peak of solar cycle 24. This suggests that haze production on Pluto (a) is driven by solar UV photons or charged particles, (b) that sources and sinks on Pluto have timescales shorter than a few Earth years, and (c) the haze precursors on Pluto are not produced by Lyman-alpha radiation, because Lyman-alpha output only decreased by about one third in between the cycle 23 and 24 peaks, much less than the observed change in Pluto's haze abundances. References: Elliot, J.L. et al. (2003) Nature, Volume 424, Issue 6945, pp. 165-168.

Pluto's Atmosphere from the 2015 June 29 Ground-based Stellar Occultation at the Time of the New Horizons Flyby

NASA Astrophysics Data System (ADS)

Sicardy, B.; Talbot, J.; Meza, E.; Camargo, J. I. B.; Desmars, J.; Gault, D.; Herald, D.; Kerr, S.; Pavlov, H.; Braga-Ribas, F.; Assafin, M.; Benedetti-Rossi, G.; Dias-Oliveira, A.; Gomes-Júnior, A. R.; Vieira-Martins, R.; Bérard, D.; Kervella, P.; Lecacheux, J.; Lellouch, E.; Beisker, W.; Dunham, D.; Jelínek, M.; Duffard, R.; Ortiz, J. L.; Castro-Tirado, A. J.; Cunniffe, R.; Querel, R.; Yock, P. C.; Cole, A. A.; Giles, A. B.; Hill, K. M.; Beaulieu, J. P.; Harnisch, M.; Jansen, R.; Pennell, A.; Todd, S.; Allen, W. H.; Graham, P. B.; Loader, B.; McKay, G.; Milner, J.; Parker, S.; Barry, M. A.; Bradshaw, J.; Broughton, J.; Davis, L.; Devillepoix, H.; Drummond, J.; Field, L.; Forbes, M.; Giles, D.; Glassey, R.; Groom, R.; Hooper, D.; Horvat, R.; Hudson, G.; Idaczyk, R.; Jenke, D.; Lade, B.; Newman, J.; Nosworthy, P.; Purcell, P.; Skilton, P. F.; Streamer, M.; Unwin, M.; Watanabe, H.; White, G. L.; Watson, D.

2016-03-01

We present results from a multi-chord Pluto stellar occultation observed on 2015 June 29 from New Zealand and Australia. This occurred only two weeks before the NASA New Horizons flyby of the Pluto system and serves as a useful comparison between ground-based and space results. We find that Pluto's atmosphere is still expanding, with a significant pressure increase of 5 ± 2% since 2013 and a factor of almost three since 1988. This trend rules out, as of today, an atmospheric collapse associated with Pluto's recession from the Sun. A central flash, a rare occurrence, was observed from several sites in New Zealand. The flash shape and amplitude are compatible with a spherical and transparent atmospheric layer of roughly 3 km in thickness whose base lies at about 4 km above Pluto's surface, and where an average thermal gradient of about 5 K km-1 prevails. We discuss the possibility that small departures between the observed and modeled flash are caused by local topographic features (mountains) along Pluto's limb that block the stellar light. Finally, using two possible temperature profiles, and extrapolating our pressure profile from our deepest accessible level down to the surface, we obtain a possible range of 11.9-13.7 μbar for the surface pressure. Partly based on observations made with the ESO WFI camera at the 2.2 m Telescope (La Silla), under program ID 079.A-9202(A) within the agreement between the ON/MCTI and the Max Planck Society, with the ESO camera NACO at the Very Large Telescope (Paranal), under program ID 089.C-0314(C), and at the Pico dos Dias Observatory/LNA, Brazil.

Re-examination of the Possibility of Haze in Pluto's Atmosphere Based on Multi-Wavelength Observations of the Pluto Occultation of P131.1.

NASA Astrophysics Data System (ADS)

Thomas-Osip, J. E.; Elliot, J. L.; Clancy, K. B.

2002-12-01

Multi-wavelength observations of the occultation of P131.1 by Pluto (see Elliot et al., this conference) allow for a re-examination of the possibility of the existence of haze in Pluto's atmosphere. Models of the extinction efficiency of haze particles as a function of wavelength are being used investigate the potential for the existence of haze in the 2002 Pluto atmosphere. The existence of a haze layer in Pluto's atmosphere was postulated to explain the abrupt change in slope seen in the light curve of the 1988 stellar occultation by Pluto (Elliot and Young 1992, AJ, 103, 991). An alternative explanation (Hubbard et al. 1990, Icarus, 84, 1) includes a steep thermal gradient near the surface instead of, or in addition to, a haze layer. Modeling of the growth and sedimentation of photo-chemically produced spherical aerosols (Stansberry et al. 1989, Geophys. Res. Let., 16, 1221) suggested that an appropriate production rate is not sufficient to produce the opacity necessary to account for change in slope found in the 1988 light curve, if it were due solely to spherical particle haze extinction. Recent studies (see for example, Rannou et al. 1995, Icarus, 188, 355 and Thomas-Osip et al. 2002, Icarus, submitted) have shown that it is likely that photochemical hazes on Titan are aggregate in nature. Fractal aggregate particles can have larger extinction efficiencies than equivalent mass spheres of the same material (Rannou et al. 1999, Planet. Space Sci., 47,385). We are, therefore, also re-examining the effect of a haze with an aggregate morphology on modeling of the 1988 occultation observations. This research has been supported in part by NSF Grant AST-0073447 and NASA Grant NAG5-10444.

Modelling Cryovolcanism Due to Subsurface Ocean Freezing on Pluto and Charon

NASA Astrophysics Data System (ADS)

Conrad, J. W.; Nimmo, F.; Singer, K. N.

2016-12-01

The New Horizons spacecraft identified various possible cryovolcanic features on the surfaces of both Pluto and Charon [1]. However, there are major differences between the cryovolcanism on Pluto and Charon. Pluto has two mound-flanked depressions which are possibly cryovolcanic [2], while Charon's putative cryovolcanism is more widespread within its smooth southern plains. If Pluto or Charon have (or had) subsurface oceans, slow refreezing of these oceans would lead to extensional surface tectonics [3,4] and pressurization of the ocean [5]. Sufficiently large pressurization can overcome the overburden pressure and cause an eruption. We applied thermal evolution models based on [3] to determine likely freezing scenarios. Eruptions on Charon are possible under most conditions, and occur after tens of kilometers of freezing of an ice shell initially 100 km thick. This would produce an areal extensional strain of 1%. The implied globally-averaged thickness of erupted material is a few hundred meters and the critical crack width for propagation through the entire ice shell [6] is about half a meter for all eruption scenarios. Eruptions on Pluto require probably unrealistic freezing scenarios, because of the larger body size and higher overburden pressure. We conclude that ocean freezing is a possible source of cryovolcanism on Charon and may explain the smooth plains in its southern hemisphere [1]. Pluto, on the other hand, requires more complex models to explain the putative cryovolcanic features on its surface. [1] Moore et al., Science 351 (2016): 1284-1293. [2] Singer et al., LPSC 47 (2016): 2276 [3] Robuchon and Nimmo, Icarus 216 (2011): 426-439. [4] Hammond et al., GRL 43 (2016). [5] Manga and Wang, GRL 34 (2007). [6] Porco et al., The Astronomical Journal 148 (2014): 45.

Craters of the Pluto-Charon System

NASA Technical Reports Server (NTRS)

Robbins, Stuart J.; Singer, Kelsi N.; Bray, Veronica J.; Schenk, Paul; Lauer, Todd R.; Weaver, Harold A.; Runyon, Kirby; Mckinnon, William B.; Beyer, Ross A.; Porter, Simon;

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. John Spencer, senior scientist at the Southwest Research Institute in Boulder, Colorado, speaks during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. John Spencer, senior scientist at the Southwest Research Institute, answers a question from the audience during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. Alan Stern, Principal Investigator on NASA's New Horizons Mission, left, delivers closing remarks following a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

Pluto: Distribution of ices and coloring agents from New Horizons LEISA observations

NASA Astrophysics Data System (ADS)

Cruikshank, Dale P.; Grundy, William M.; Stern, S. Alan; Olkin, Catherine B.; Cook, Jason C.; Dalle Ore, Cristina M.; Binzel, Richard P.; Earle, Alissa M.; Ennico, Kimberly; Jennings, Donald E.; Howett, Carly J. A.; Linscott, Ivan R.; Lunsford, Allen W.; Parker, Alex H.; Parker, Joel W.; Protopapa, Silvia; Reuter, Dennis C.; Singer, Kelsi N.; Spencer, John R.; Tsang, Constantine C. C.; Verbiscer, Anne J.; Weaver, Harold A.; Young, Leslie A.

2015-11-01

Pluto was observed at high spatial resolution (maximum ~3 km/px) by the New Horizons LEISA imaging spectrometer. LEISA is a component of the Ralph instrument (Reuter, D.C., Stern, S.A., Scherrer, J., et al. 2008, Space Sci. Rev. 140, 129) and affords a spectral resolving power of 240 in the wavelength range 1.25-2.5 µm, and 560 in the range 2.1-2.25 µm. Spatially resolved spectra with LEISA are used to map the distributions of the known ices on Pluto (N2, CH4, CO) and to search for other surface components. The spatial distribution of volatile ices is compared with the distribution of the coloring agent(s) on Pluto's surface. The correlation of ice abundance and the degree of color (ranging from yellow to orange to dark red) is consistent with the presence of tholins, which are refractory organic solids of complex structure and high molecular weight, with colors consistent with those observed on Pluto. Tholins are readily synthesized in the laboratory by energetic processing of mixtures of the ices (N2, CH4, CO) known on Pluto's surface. We present results returned from the spacecraft to date obtained from the analysis of the high spatial resolution dataset obtained near the time of closest approach to the planet. Supported by NASA’s New Horizons project.

Pluto Haze in Bands of Blue

NASA Image and Video Library

2016-01-14

This processed image is the highest-resolution color look yet at the haze layers in Pluto's atmosphere. Shown in approximate true color, the picture was constructed from a mosaic of four panchromatic images from the Long Range Reconnaissance Imager (LORRI) splashed with Ralph/Multispectral Visible Imaging Camera (MVIC) four-color filter data, all acquired by NASA's New Horizons spacecraft on July 14, 2015. The resolution is 1 kilometer (0.6 miles) per pixel; the sun illuminates the scene from the right. Scientists believe the haze is a photochemical smog resulting from the action of sunlight on methane and other molecules in Pluto's atmosphere, producing a complex mixture of hydrocarbons such as acetylene and ethylene. These hydrocarbons accumulate into small particles, a fraction of a micrometer in size, and scatter sunlight to make the bright blue haze seen in this image. As they settle down through the atmosphere, the haze particles form numerous intricate, horizontal layers, some extending for hundreds of miles around Pluto. The haze layers extend to altitudes of over 200 kilometers (120 miles). Adding to the stark beauty of this image are mountains on Pluto's limb (on the right, near the 4 o'clock position), surface features just within the limb to the right, and crepuscular rays (dark finger-like shadows to the left) extending from Pluto's topographic features. http://photojournal.jpl.nasa.gov/catalog/PIA20362

A Pluto-like radius and a high albedo for the dwarf planet Eris from an occultation.

PubMed

Sicardy, B; Ortiz, J L; Assafin, M; Jehin, E; Maury, A; Lellouch, E; Hutton, R Gil; Braga-Ribas, F; Colas, F; Hestroffer, D; Lecacheux, J; Roques, F; Santos-Sanz, P; Widemann, T; Morales, N; Duffard, R; Thirouin, A; Castro-Tirado, A J; Jelínek, M; Kubánek, P; Sota, A; Sánchez-Ramírez, R; Andrei, A H; Camargo, J I B; da Silva Neto, D N; Gomes, A Ramos; Martins, R Vieira; Gillon, M; Manfroid, J; Tozzi, G P; Harlingten, C; Saravia, S; Behrend, R; Mottola, S; Melendo, E García; Peris, V; Fabregat, J; Madiedo, J M; Cuesta, L; Eibe, M T; Ullán, A; Organero, F; Pastor, S; de Los Reyes, J A; Pedraz, S; Castro, A; de la Cueva, I; Muler, G; Steele, I A; Cebrián, M; Montañés-Rodríguez, P; Oscoz, A; Weaver, D; Jacques, C; Corradi, W J B; Santos, F P; Reis, W; Milone, A; Emilio, M; Gutiérrez, L; Vázquez, R; Hernández-Toledo, H

2011-10-26

The dwarf planet Eris is a trans-Neptunian object with an orbital eccentricity of 0.44, an inclination of 44 degrees and a surface composition very similar to that of Pluto. It resides at present at 95.7 astronomical units (1 AU is the Earth-Sun distance) from Earth, near its aphelion and more than three times farther than Pluto. Owing to this great distance, measuring its size or detecting a putative atmosphere is difficult. Here we report the observation of a multi-chord stellar occultation by Eris on 6 November 2010 UT. The event is consistent with a spherical shape for Eris, with radius 1,163 ± 6 kilometres, density 2.52 ± 0.05 grams per cm(3) and a high visible geometric albedo, Pv = 0.96(+0.09)(-0.04). No nitrogen, argon or methane atmospheres are detected with surface pressure larger than ∼1 nanobar, about 10,000 times more tenuous than Pluto's present atmosphere. As Pluto's radius is estimated to be between 1,150 and 1,200 kilometres, Eris appears as a Pluto twin, with a bright surface possibly caused by a collapsed atmosphere, owing to its cold environment. We anticipate that this atmosphere may periodically sublimate as Eris approaches its perihelion, at 37.8 astronomical units from the Sun.

Platform technology for scalable assembly of instantaneously functional mosaic tissues

PubMed Central

Zhang, Boyang; Montgomery, Miles; Davenport-Huyer, Locke; Korolj, Anastasia; Radisic, Milica

2015-01-01

Engineering mature tissues requires a guided assembly of cells into organized three-dimensional (3D) structures with multiple cell types. Guidance is usually achieved by microtopographical scaffold cues or by cell-gel compaction. The assembly of individual units into functional 3D tissues is often time-consuming, relying on cell ingrowth and matrix remodeling, whereas disassembly requires an invasive method that includes either matrix dissolution or mechanical cutting. We invented Tissue-Velcro, a bio-scaffold with a microfabricated hook and loop system. The assembly of Tissue-Velcro preserved the guided cell alignment realized by the topographical features in the 2D scaffold mesh and allowed for the instant establishment of coculture conditions by spatially defined stacking of cardiac cell layers or through endothelial cell coating. The assembled cardiac 3D tissue constructs were immediately functional as measured by their ability to contract in response to electrical field stimulation. Facile, on-demand tissue disassembly was demonstrated while preserving the structure, physical integrity, and beating function of individual layers. PMID:26601234

Impact of different disassembly line balancing algorithms on the performance of dynamic kanban system for disassembly line

NASA Astrophysics Data System (ADS)

Kizilkaya, Elif A.; Gupta, Surendra M.

2005-11-01

In this paper, we compare the impact of different disassembly line balancing (DLB) algorithms on the performance of our recently introduced Dynamic Kanban System for Disassembly Line (DKSDL) to accommodate the vagaries of uncertainties associated with disassembly and remanufacturing processing. We consider a case study to illustrate the impact of various DLB algorithms on the DKSDL. The approach to the solution, scenario settings, results and the discussions of the results are included.

Haze Production in Pluto's Atmosphere

NASA Astrophysics Data System (ADS)

Summers, M. E.; Gladstone, R.; Stern, A.; Ennico Smith, K.; Greathouse, T.; Hinson, D. P.; Kammer, J.; Linscott, I.; Olkin, C.; Parker, A. H.; Parker, J. W.; Retherford, K. D.; Schindhelm, E.; Singer, K. N.; Steffl, A.; Strobel, D. F.; Tsang, C.; Tyler, G. L.; Versteeg, M. H.; Weaver, H. A., Jr.; Wong, M. L.; Woods, W. W.; Yung, Y. L.; Young, L. A.; Lisse, C. M.; Lavvas, P.; Renaud, J.; Ewell, M.; Jacobs, A. D.

2015-12-01

One of the most visible manifestations of Pluto's atmosphere observed from the New Horizons spacecraft during the flyby in July 2015 was a global haze layer extending to an altitude ~150 km above Pluto's surface. The haze layer exhibits a significant hemispheric asymmetry and what appears to be layered and/or wave like features. Stellar observations since 1989 have suggested the existence of a haze layer in Pluto's lower atmosphere to explain features in occultation light curves. A haze layer is also expected from photochemical models of Pluto's methane atmosphere wherein hydrocarbons and are produced at altitudes above 100 km altitude, mix downwards, and condense at the low atmospheric temperatures near the surface. However, the observed haze layer(s) extends much higher where the atmospheric temperature is too high for condensation. In this paper we will discuss the production and condensation of photochemical products, and evaluate the possibility that nucleation begins in the ionosphere by a mechanism similar to that proposed for the atmosphere of Titan, where electron attachments initiates a sequence of ion-molecular reactions that ultimately produce aerosol "tholins" that settle downward and coat the surface.

Radio Occultation Measurements of Pluto’s Atmosphere with New Horizons

NASA Astrophysics Data System (ADS)

Hinson, David P.; Linscott, Ivan; Tyler, Len; Bird, Mike; Paetzold, Martin; Strobel, Darrell; Summers, Mike; Woods, Will; Stern, Alan; Weaver, Hal; Olkin, Cathy; Young, Leslie; Ennico, Kimberly; Gladstone, Randy; Greathouse, Tommy; Kammer, Josh; Parker, Alex; Parker, Joel; Retherford, Kurt; Schindhelm, Eric; Singer, Kelsi; Steffl, Andrew; Tsang, Con; Versteeg, Maarten

2015-11-01

The reconnaissance of the Pluto System by New Horizons included radio occultations at both Pluto and Charon. This talk will present the latest results from the Pluto occultation. The REX instrument onboard New Horizons received and recorded uplink signals from two 70-m antennas and two 34-m antennas of the NASA Deep Space Network - each transmitting 20 kW at 4.2-cm wavelength - during a diametric occultation by Pluto. At the time this was written only a short segment of data at occultation entry (193°E, 17°S) was available for analysis. The REX measurements extend unequivocally to the surface, providing the first direct measure of the surface pressure and the temperature structure in Pluto’s lower atmosphere. Data from occultation exit (16°E, 15°N) are scheduled to arrive on the ground in late August 2015. Those observations will yield an improved estimate of the surface pressure, a second temperature profile, and a measure of the diameter of Pluto with a precision of a few hundred meters. This work is supported by the NASA New Horizons Mission.

Topographic Mapping of Pluto and Charon Using New Horizons Data

NASA Astrophysics Data System (ADS)

Schenk, P. M.; Beyer, R. A.; Moore, J. M.; Spencer, J. R.; McKinnon, W. B.; Howard, A. D.; White, O. M.; Umurhan, O. M.; Singer, K.; Stern, S. A.; Weaver, H. A.; Young, L. A.; Ennico Smith, K.; Olkin, C.; Horizons Geology, New; Geophysics Imaging Team

2016-06-01

New Horizons 2015 flyby of the Pluto system has resulted in high-resolution topographic maps of Pluto and Charon, the most distant objects so mapped. DEM's over ~30% of each object were produced at 100-300 m vertical and 300-800 m spatial resolutions, in hemispheric maps and high-resolution linear mosaics. Both objects reveal more relief than was observed at Triton. The dominant 800-km wide informally named Sputnik Planum bright ice deposit on Pluto lies in a broad depression 3 km deep, flanked by dispersed mountains 3-5 km high. Impact craters reveal a wide variety of preservation states from pristine to eroded, and long fractures are several km deep with throw of 0-2 km. Topography of this magnitude suggests the icy shell of Pluto is relatively cold and rigid. Charon has global relief of at least 10 km, including ridges of 2-3 km and troughs of 3-5 km of relief. Impact craters are up to 6 km deep. Vulcan Planum consists of rolling plains and forms a topographic moat along its edge, suggesting viscous flow.

The geology of Pluto and Charon through the eyes of New Horizons.

PubMed

Moore, Jeffrey M; McKinnon, William B; Spencer, John R; Howard, Alan D; Schenk, Paul M; Beyer, Ross A; Nimmo, Francis; Singer, Kelsi N; Umurhan, Orkan M; White, Oliver L; Stern, S Alan; Ennico, Kimberly; Olkin, Cathy B; Weaver, Harold A; Young, Leslie A; Binzel, Richard P; Buie, Marc W; Buratti, Bonnie J; Cheng, Andrew F; Cruikshank, Dale P; Grundy, Will M; Linscott, Ivan R; Reitsema, Harold J; Reuter, Dennis C; Showalter, Mark R; Bray, Veronica J; Chavez, Carrie L; Howett, Carly J A; Lauer, Tod R; Lisse, Carey M; Parker, Alex Harrison; Porter, S B; Robbins, Stuart J; Runyon, Kirby; Stryk, Ted; Throop, Henry B; Tsang, Constantine C C; Verbiscer, Anne J; Zangari, Amanda M; Chaikin, Andrew L; Wilhelms, Don E

2016-03-18

NASA's New Horizons spacecraft has revealed the complex geology of Pluto and Charon. Pluto's encounter hemisphere shows ongoing surface geological activity centered on a vast basin containing a thick layer of volatile ices that appears to be involved in convection and advection, with a crater retention age no greater than ~10 million years. Surrounding terrains show active glacial flow, apparent transport and rotation of large buoyant water-ice crustal blocks, and pitting, the latter likely caused by sublimation erosion and/or collapse. More enigmatic features include tall mounds with central depressions that are conceivably cryovolcanic and ridges with complex bladed textures. Pluto also has ancient cratered terrains up to ~4 billion years old that are extensionally faulted and extensively mantled and perhaps eroded by glacial or other processes. Charon does not appear to be currently active, but experienced major extensional tectonism and resurfacing (probably cryovolcanic) nearly 4 billion years ago. Impact crater populations on Pluto and Charon are not consistent with the steepest impactor size-frequency distributions proposed for the Kuiper belt. Copyright © 2016, American Association for the Advancement of Science.

The Geology of Pluto and Charon Through the Eyes of New Horizons

NASA Technical Reports Server (NTRS)

Moore, Jeffrey M.; McKinnon, William B.; Spencer, John R.; Howard, Alan D.; Schenk, Paul M.; Beyer, Ross A.; Nimmo, Francis; Singer, Kelsi N.; Umurhan, Orkan M.; White, Oliver L.;

Understanding Pluto's Surface: Correlations between Geology and Composition

NASA Astrophysics Data System (ADS)

Spencer, J. R.; Stern, A.; Weaver, H. A., Jr.; Young, L. A.; Olkin, C.; Ennico Smith, K.; Moore, J. M.; Grundy, W. M.

2015-12-01

New Horizons has revealed that Pluto's surface is composed of a remarkable variety of terrains that differ strikingly in their landforms, color, and near-infrared spectral characteristics. Strong correlations are seen between the morphology revealed by high-resolution imaging from the Long Range Reconnaissance Imager (LORRI), and the surface composition inferred from the spacecraft's color camera and near-infrared spectrometer, which are both included in the Ralph instrument. These correlations provide the potential for a much deeper understanding of the processes that have shaped Pluto's complex surface that was possible for Pluto's sibling Triton, for which Voyager did not provide compositional maps. We will discuss how the full suite of New Horizons remote sensing instruments reveal a surface modified by the interplay of insolation variations, meteorology, and endogenic processes.

New Horizons arrives at Pluto on This Week @NASA – July 17, 2015

NASA Image and Video Library

2015-07-17

After a nearly decade-long journey, NASA’s New Horizons spacecraft arrived at Pluto on July 14 – passing by at a mere 7,750 miles above the surface … resulting in an absolutely breathtaking image – the closest ever of Pluto. Initial congratulations included a Twitter post from the White House … and from iconic figures in the scientific community. The so-called “data waterfall” released by New Horizons contains so many astounding images and detailed information about Pluto that investigators anticipate it will take about 16 months to send it all back to Earth. Also, Mariner 4 Mars flyby anniversary, Newman sworn-in, New wildfire detection tool, Expedition 44/45 prepares for launch and 40th anniversary of Apollo-Soyuz!

The Surface Age of Sputnik Planum, Pluto, Must Be Less than 10 Million Years

PubMed Central

Trilling, David E.

2016-01-01

Data from the New Horizons mission to Pluto show no craters on Sputnik Planum down to the detection limit (2 km for low resolution data, 625 m for high resolution data). The number of small Kuiper Belt Objects that should be impacting Pluto is known to some degree from various astronomical surveys. We combine these geological and telescopic observations to make an order of magnitude estimate that the surface age of Sputnik Planum must be less than 10 million years. This maximum surface age is surprisingly young and implies that this area of Pluto must be undergoing active resurfacing, presumably through some cryo-geophysical process. We discuss three possible resurfacing mechanisms and the implications of each one for Pluto’s physical properties. PMID:26790001

Family Portrait of Pluto Moons

NASA Image and Video Library

2015-10-23

This composite image shows a sliver of Pluto large moon, Charon, and all four of Pluto small moons, as resolved by the Long Range Reconnaissance Imager (LORRI) on the New Horizons spacecraft. All the moons are displayed with a common intensity stretch and spatial scale (see scale bar). Charon is by far the largest of Pluto's moons, with a diameter of 751 miles (1,212 kilometers). Nix and Hydra have comparable sizes, approximately 25 miles (40 kilometers) across in their longest dimension above. Kerberos and Styx are much smaller and have comparable sizes, roughly 6-7 miles (10-12 kilometers) across in their longest dimension. All four small moons have highly elongated shapes, a characteristic thought to be typical of small bodies in the Kuiper Belt. http://photojournal.jpl.nasa.gov/catalog/PIA20033

Pluto and the platypus: An odd ball and an odd duck - On classificatory norms.

PubMed

Slater, Matthew H

2017-02-01

Many astronomers seem to believe that we have discovered that Pluto is not a planet. I contest this assessment. Recent discoveries of trans-Neptunian Pluto-sized objects do not militate for Pluto's expulsion from the planets unless we have prior reason for not simply counting these newly-discovered objects among the planets. I argue that this classificatory controversy - which I compare to the controversy about the classification of the platypus - illustrates how our classificatory practices are laden with normative commitments of a distinctive kind. I conclude with a discussion of the relevance of such "norm-ladenness" to other controversies in the metaphysics of classification, such as the monism/pluralism debate. Copyright © 2017 The Author. Published by Elsevier Ltd.. All rights reserved.

To Pluto by way of a postage stamp

NASA Technical Reports Server (NTRS)

Staehle, Robert L.; Terrile, Richard J.; Weinstein, Stacy S.

1994-01-01

In this time of constrained budgets, the primary question facing planetary explorers is not 'Can we do it?' but 'Can we do it cheaply?' Taunted by words on a postage stamp, a group of mission designers at the Jet Propulsion Laboratory is struggling to find a cheap way to go to Pluto. Three primary goals were set by the science community: (1) imaging of Pluto and Charon, (2) mapping their surface composition, and (3) characterizing Pluto's atmosphere. The spacecraft will be designed around these primary goals. With the help of the Advanced Technology Insertion (ATI) process $5 million was alloted for two years to shop for lightweight components and subsystems using new technology never tried on a planetary mission. The process for this search and development is described.

The Color of Pluto from New Horizons

NASA Astrophysics Data System (ADS)

Olkin, Catherine; Spencer, John R.; Grundy, William M.; Parker, Alex; Beyer, Ross A.; Reuter, Dennis; Schenk, Paul M.; Stern, S. Alan; Weaver, Harold A.; Young, Leslie; Ennico, Kimberly; Binzel, Richard P.; Buie, Marc W.; Cook, Jason C.; Cruikshank, Dale P.; Dalle Ore, Cristina M.; Earle, Alissa; Howett, Carly; Jennings, Donald E.; Singer, Kelsi N.; Linscott, Ivan; Lunsford, Allen; Protopapa, Silvia; Schmitt, Bernard; Weigle, Eddie; and the New Horizons Science Team

2017-10-01

The New Horizons flyby provided the first high-resolution color maps of Pluto. These maps show the color variegation across the surface from the very red terrain in the equatorial region, to the more neutral colors of the volatile ices in Sputnik Planitia, the blue terrain of east Tombaugh Regio and the yellow hue on Pluto's north pole. There are two distinct color mixing lines in the color-color diagrams derived from images of Pluto. Both mixing lines have an apparent starting point in common: the relatively neutral color volatile-ice covered terrain. One line extends to the dark red terrain exemplified by Cthulu Regio and the other extends to the yellow hue in the northern latitudes. The red color is consistent with a non-ice component on the surface and is consistent with tholins.

Closer Look: Majestic Mountains and Frozen Plains

NASA Image and Video Library

2015-09-17

Just 15 minutes after its closest approach to Pluto on July 14, 2015, NASA's New Horizons spacecraft looked back toward the sun and captured a near-sunset view of the rugged, icy mountains and flat ice plains extending to Pluto's horizon. The smooth expanse of the informally named Sputnik Planum (right) is flanked to the west (left) by rugged mountains up to 11,000 feet (3,500 meters) high, including the informally named Norgay Montes in the foreground and Hillary Montes on the skyline. The backlighting highlights more than a dozen layers of haze in Pluto's tenuous but distended atmosphere. The image was taken from a distance of 11,000 miles (18,000 kilometers) to Pluto; the scene is 230 miles (380 kilometers) across. http://photojournal.jpl.nasa.gov/catalog/PIA19947

Formation of the Sputnik Planum basin and the thickness of Pluto's subsurface ocean

NASA Astrophysics Data System (ADS)

Johnson, Brandon C.; Bowling, Timothy J.; Trowbridge, Alexander J.; Freed, Andrew M.

2016-10-01

We simulate the formation of the large elliptical impact basin associated with Pluto's Sputnik Planum (SP; informal name). The location of SP suggests that it represents a large positive mass anomaly. To find the conditions necessary for SP to have a positive mass anomaly, we consider impacts into targets with a range of thermal states and ocean thicknesses. Assuming the basin evolves to its current-day configuration, we calculate the mass and gravity anomalies associated with SP. We find that SP can only achieve a large positive mass anomaly if Pluto has a more than 100 km thick salty ocean. This conclusion may help us better understand the composition and thermal evolution of Pluto. Furthermore, our work supports the hypothesis that SP basin has an impact origin.

The Color of Pluto from New Horizons

NASA Astrophysics Data System (ADS)

Olkin, C.; Spencer, J. R.; Grundy, W. M.; Parker, A. H.; Beyer, R. A.; Reuter, D.; Schenk, P.; Stern, A.; Weaver, H. A., Jr.; Young, L. A.; Ennico Smith, K.

2017-12-01

The New Horizons flyby provided the first high-resolution color maps of Pluto. These maps show the color variegation across the surface from the very red terrain in the equatorial region, to the more neutral colors of the volatile ices in Sputnik Planitia, the blue terrain of east Tombaugh Regio and the yellow hue on Pluto's north pole. There are two distinct color mixing lines in the color-color diagrams derived from images of Pluto. Both mixing lines have an apparent starting point in common: the relatively neutral color volatile-ice covered terrain. One line extends to the dark red terrain exemplified by Cthulu Regio and the other extends to the yellow hue in the northern latitudes. The red color is consistent with a non-ice component on the surface and is consistent with tholins.

The Small Satellites of Pluto as Observed by New Horizons

NASA Technical Reports Server (NTRS)

Weaver, H. A.; Buie, M. W; Buratti, B. J.; Grundy, W. M.; Lauer, T. R.; Olkin, C. B.; Parker, A .H.; Porter, S. B.; Showalter, M. R.; Spencer, J. R.;

Computational algorithm to evaluate product disassembly cost index

NASA Astrophysics Data System (ADS)

Zeid, Ibrahim; Gupta, Surendra M.

2002-02-01

Environmentally conscious manufacturing is an important paradigm in today's engineering practice. Disassembly is a crucial factor in implementing this paradigm. Disassembly allows the reuse and recycling of parts and products that reach their death after their life cycle ends. There are many questions that must be answered before a disassembly decision can be reached. The most important question is economical. The cost of disassembly versus the cost of scrapping a product is always considered. This paper develops a computational tool that allows decision-makers to calculate the disassembly cost of a product. The tool makes it simple to perform 'what if' scenarios fairly quickly. The tool is Web based and has two main parts. The front-end part is a Web page and runs on the client side in a Web browser, while the back-end part is a disassembly engine (servlet) that has disassembly knowledge and costing algorithms and runs on the server side. The tool is based on the client/server model that is pervasively utilized throughout the World Wide Web. An example is used to demonstrate the implementation and capabilities of the tool.

The "Geology" of Pluto and Charon

NASA Astrophysics Data System (ADS)

Moore, J. M.; Schenk, P. M.; Pappalardo, R. T.; McKinnon, W. B.

2003-04-01

To speculate about the geology of Pluto and Charon with currently available data is very risky. It is important to remember that we would anticipate that Ganymede and Callisto might have very similar geologies, given the same level of understanding, as we presently possess for the Pluto system. What little we do know with regards to Pluto and Charon's composition, surface albedo variations, and in combination with a post-Voyager and Galileo appreciation of other outer solar system icy objects, at least establishes a criteria for identifying geological questions we wish to address with the upcoming New Horizons mission to that system. Here we give a few examples. Tectonics: Pluto and Charon's geologic history may have involved periods of internal expansion and/or contraction, perhaps due to a build-up of heat from radiogenic sources, the freeze-expansion of a large internal H2O layer, or changes in ice phases. Global internal expansion would manifest itself of the surfaces of these objects in the form of normal faulting and graben formation causing the surface to split into scarp or graben-bounded polygons. Global compression would form a network of thrust fault ridges. Orbital evolution also may have left tectonic imprints. Volcanics : The Voyager survey of the outer solar system has revealed an astonishing variety of endogenic landforms on the surfaces of icy satellites. If Pluto or Charon exhibit evidence of volcanic activity, such observations can be used to constrain composition and thermal evolutions. On Triton, a possible form of active outgassing, whether from deep or shallow sources is a matter of controversy, was observed in the form of narrow plumes. Alternative models for Tritonian plume genesis can be tested by their occurrence on Pluto. Cratering: The presumed absence of any additional heating other than radiogenic may have resulted in the preservation of older (hence more cratered) terrains on Pluto and Charon than on Triton, which would be a boon to the study of time-varying trans-Neptunian bolide populations. Aeolian Activity: For the "densest case" Plutonian atmosphere (˜50 μbar surface pressure), the saltation threshold wind speed is in the range of maximum theoretical surface wind speeds. The observation of landforms created by saltating particles (e.g., dunes) may provide an indicator of periods of high (>= 50 μbar) atmospheric pressures. This may be an especially useful observation if post-perihelion in situ measurements detect a significantly smaller atmosphere. Looking toward an opportunity to send spacecraft to the Pluto-Charon system has encouraged this speculation regarding geological processes and the implications of their presence/absence on these bodies. Finally we should anticipate observing wholly unexpected features on the surfaces of Pluto and Charon in any initial in situ spacecraft investigation.

Multikanban model for disassembly line with demand fluctuation

NASA Astrophysics Data System (ADS)

Udomsawat, Gun; Gupta, Surendra M.; Al-Turki, Yousef A. Y.

2004-02-01

In recent years, the continuous growth in consumer waste and dwindling natural resources has seriously threatened the environment. Realizing this, several countries have passed regulations that force manufacturers not only to manufacture environmentally conscious products, but also to take back their used products from consumers so that the components and materials recovered from the products may be reused and/or recycled. Disassembly plays an important role in product recovery. A disassembly line is perhaps the most suitable setting for disassembly of products in large quantities. Because a disassembly line has a tendency to generate excessive inventory, employing a kanban system can reduce the inventory level and let the system run more efficiently. A disassembly line is quite different from an assembly line. For example, not only can the demand arrive at the last station, it can also arrive at any of the other stations in the system. The demand for a component on the disassembly line could fluctuate widely. In fact, there are many other complicating matters that need to be considered to implement the concept of kanbans in such an environment. In this paper, we discuss the complications that are unique to a disassembly line. We discuss the complications in utilizing the conventional production control mechanisms in a disassembly line setting. We then show how to overcome them by implementing kanbans in a disassembly line setting with demand fluctuation and introduce the concept of multi-kanban mechanism. We demonstrate its effectiveness using a simulation model. An example is presented to illustrate the concept.

Pluto.

ERIC Educational Resources Information Center

Binzel, Richard P.

1990-01-01

Discussed are details of what is known about the composition, physical characteristics, and formation of the planet Pluto and its satellite, Charon. Alignments of these bodies and details of their rotations and revolutions are described. (CW)

Blades Across Pluto

NASA Image and Video Library

2016-03-31

The red outline in this global view of Pluto from NASA New Horizons marks the large area of mysterious, bladed terrain extending from the eastern section of the large feature informally named Tombaugh Regio.

Optical Navigation Preparations for New Horizons Pluto Flyby

NASA Technical Reports Server (NTRS)

Owen, William M., Jr.; Dumont, Philip J.; Jackman, Coralie D.

2012-01-01

The New Horizons spacecraft will encounter Pluto and its satellites in July 2015. As was the case for the Voyager encounters with Jupiter, Saturn, Uranus and Neptune, mission success will depend heavily on accurate spacecraft navigation, and accurate navigation will be impossible without the use of pictures of the Pluto system taken by the onboard cameras. We describe the preparations made by the New Horizons optical navigators: picture planning, image processing algorithms, software development and testing, and results from in-flight imaging.

Pluto in True Color

NASA Image and Video Library

2015-07-25

Four images from NASA's New Horizons' Long Range Reconnaissance Imager (LORRI) were combined with color data from the Ralph instrument to create this global view of Pluto. (The lower right edge of Pluto in this view currently lacks high-resolution color coverage.) The images, taken when the spacecraft was 280,000 miles (450,000 kilometers) away, show features as small as 1.4 miles (2.2 kilometers), twice the resolution of the single-image view taken on July 13. http://photojournal.jpl.nasa.gov/catalog/PIA19857

Effects of UAVS on Interstate Relationships: A Case Study of U.S. Relations with Pakistan and Yemen

DTIC Science & Technology

2015-06-01

ed. Usama Butt and Julian Schofield (New York: Pluto Press, 2012), 46–47. 87. Christophe Jaffrelot, A History of Pakistan and its Origins (London...Grand Strategies, ed. Usama Butt and Julian Schofield (New York: Pluto Press, 2012), 111–112. 100. Rubin, “Realities Collide,” 56; Rajeev Sharma...Schofield. New York: Pluto Press, 2012. 110–129. Al Ahmad, Safa. “The Fight for Yemen.” Frontline, PBS, April 7, 2015. http://www.pbs.org/wgbh

High-resolution imaging of the Pluto-Charon system with the Faint Object Camera of the Hubble Space Telescope

NASA Technical Reports Server (NTRS)

Albrecht, R.; Barbieri, C.; Adorf, H.-M.; Corrain, G.; Gemmo, A.; Greenfield, P.; Hainaut, O.; Hook, R. N.; Tholen, D. J.; Blades, J. C.

1994-01-01

Images of the Pluto-Charon system were obtained with the Faint Object Camera (FOC) of the Hubble Space Telescope (HST) after the refurbishment of the telescope. The images are of superb quality, allowing the determination of radii, fluxes, and albedos. Attempts were made to improve the resolution of the already diffraction limited images by image restoration. These yielded indications of surface albedo distributions qualitatively consistent with models derived from observations of Pluto-Charon mutual eclipses.

Color Image of Pluto

NASA Image and Video Library

2015-12-31

Pluto nearly fills the frame in this image from the Long Range Reconnaissance Imager (LORRI) aboard New Horizons, taken on July 13, 2015, when the spacecraft was 476,000 miles (768,000 kilometers) from the surface. This is the last and most detailed image sent to Earth before the spacecraft's closest approach to Pluto on July 14. The color image has been combined with lower-resolution color information from the Ralph instrument that was acquired earlier on July 13. http://photojournal.jpl.nasa.gov/catalog/PIA20291

Solid methane on Triton and Pluto - 3- to 4-micron spectrophotometry

NASA Technical Reports Server (NTRS)

Spencer, John R.; Buie, Marc W.; Bjoraker, Gordon L.

1990-01-01

Methane has been identified in the Pluto/Charon system on the basis of absorption features in the reflectance spectrum at 1.5 and 2.3 microns; attention is presently given to observations of a 3.25 micron-centered deep absorption feature in Triton and Pluto/Charon system reflectance spectra. This absorption may indicate the presence of solid methane, constituting either the dominant surface species or a mixture with a highly transparent substance, such as N2 frost.

Attività fotometrica di Plutone nel 2005

NASA Astrophysics Data System (ADS)

Bianciardi, Giorgio

2006-06-01

This report describes unfiltered CCD differential photometry of Pluto performed between 1 August and 10 September 2005. Results show that in the present year Pluto is maintaining a high photometric activity, higher than expected (maximum brightness variations of 0.29±0.02 magnitudes) in relation to the rotational period. Pluto's appearance is now drastically changing owing to viewing geometry and the next collapse of its atmosphere onto the surface. Amateurs too should dedicate particular attention to the photometric evolution of the planet.

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. David H. Grinspoon, senior scientist at the Planetary Science Institute, speaks about working on NASA's Voyager team while serving as moderator for a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

Pluto Fretted Terrain

NASA Image and Video Library

2016-05-20

NASA New Horizons scientists have spotted an expanse of terrain they describe as fretted bright plains divided into polygon-shaped blocks by a network of dark, connected valleys in Pluto informally named Venera Terra region.

Spectroscopy of Pluto, 380-930 Nm at Six Longitudes

NASA Technical Reports Server (NTRS)

Cruikshank, D. P.; Pinilla-Alonso, N.; Lorenzi, V.; Grundy, William; Licandro, J.; Binzel, R. P.

2014-01-01

We have obtained spectra of the Pluto-Charon pair (unresolved) in the wavelength range 380-930 nm with resolution approx..450 at six roughly equally spaced longitudes. The data were taken in May and June, 2014, with the 4.2-m Isaac Newton Telescope at Roque de Los Muchachos Observatory in the Canary Islands, using the ACAM (auxiliary-port camera) in spectrometer mode, and using two solar analog stars. The new spectra clearly show absorption bands of solid CH4 at 620, 728, and 850-910 nm, which were known from earlier work. The 620-nm CH4 band is intrinsically very weak, and its appearance indicates a long optical path-length through the ice. This is especially true if it arises from CH4 dissolved in N2 ice. Earlier work (Owen et al. Science 261, 745, 1993) on the near-infrared spectrum of Pluto (1-2.5 microns) has shown that the CH4 bands are shifted to shorter wavelengths because the CH4 occurs as a solute in beta-phase crystalline N2. The optical path-length through the N2 crystals must be on the order of several cm to produce the N2 band observed at 2.15 microns. The new spectra exhibit a pronounced red slope across the entire wavelength range; the slope is variable with longitude, and differs in a small but significant way from that measured at comparable longitudes by Grundy & Fink (Icarus 124, 329, 1996) in their 15-year study of Pluto's spectrum (500-1000 nm). The new spectra will provide an independent means for calibrating the color filter bands on the Multispectral Visible Imaging Camera (MVIC) (Reuter et al. Space Sci. Rev. 140, 129, 2008) on the New Horizons spacecraft, which will encounter the Pluto-Charon system in mid-2015. They will also form the basis of modeling the spectrum of Pluto at different longitudes to help establish the nature of the non-ice component(s) of Pluto's surface. It is presumed that the non-ice component is the source of the yellow-red coloration of Pluto, which is known to be variable across the surface.

Pluto's Atmosphers

NASA Astrophysics Data System (ADS)

Elliot, J. L.

2002-09-01

Pluto's tenuous atmosphere -- detected with a widely observed stellar occultation in 1988 (Millis et al., 1993, Icarus 105, 282) -- consists primarily of N2, with trace amounts of CO and CH4. The N2 gas is in vapor-pressure equilibrium with surface ice, which should maintain a uniform temperature for the N2 ice on the surface of the body. Data from the Kuiper Airborne Observatory (KAO) for the 1988 occultation showed Pluto's middle atmosphere to be isothermal at about 105 K for at least a scale height above a radius of about 1215 km (Pluto's surface radius is 1175 +/- 25 km; Tholen & Buie 1997, in Pluto and Charon, 193). This temperature can be explained with radiative-conductive models (e.g. Yelle & Lunine 1989, Nature 339, 288; Strobel et al. 1996, Icarus 120 266), using the spectroscopically measured amount of CH4 (Young et al. 1997, Icarus, 127 258). Below the isothermal region there is an abrupt drop in the KAO occultation light curve, which has been interpreted as being caused either by (i) an absorption layer, or (ii) a sharp thermal gradient. As Pluto recedes from the sun, the diminishing solar flux provides less energy for sublimation, which may lead to a substantial drop in surface pressure. On the other hand, the emissivity change that accompanies the α - β phase transition for N2 ice may leave the surface pressure relatively unchanged from its present value (Stansberry & Yelle 1999, Icarus 141, 299). Stellar occultation observations were successfully carried out in 2002 July and August (Sicardy et al., Buie et al., and Elliot et al., this conference) from a large number of telescopes: the IRTF, UH 2.2 m, UH 0.6 m, UKIRT, CFHT, Lick 3 m, Lowell 1.8 m, Palomar 5 m, as well as 0.35 m and smaller portable telescopes. The wavelengths of these observations ranged from the visible to near IR. These new data give us a snapshot of Pluto's atmospheric structure 14 years after the initial observations and reveal changes in the structure of Pluto's atmosphere. Occultation research at MIT is supported, in part, by NASA (NAG5-10444) and NSF (AST-0073447).

Pluto and it's moon Charon Shine in False Color

NASA Image and Video Library

2017-12-08

**This image was taken at 3:38 a.m. EDT on July 13, one day before New Horizons’ closest approach to Pluto.** New Horizons has obtained impressive new images of Pluto and its large moon Charon that highlight their compositional diversity. These are not actual color images of Pluto and Charon—they are shown here in exaggerated colors that make it easy to note the differences in surface material and features on each planetary body. The images were obtained using three of the color filters of the “Ralph” instrument on July 13 at 3:38 am EDT. New Horizons has seven science instruments on board the spacecraft—including “Ralph” and “Alice”, whose names are a throwback to the “Honeymooners,” a popular 1950s sitcom. “These images show that Pluto and Charon are truly complex worlds. There's a whole lot going on here,” said New Horizons co-investigator Will Grundy, Lowell Observatory, Flagstaff, Arizona. “Our surface composition team is working as fast as we can to identify the substances in different regions on Pluto and unravel the processes that put them where they are.” The color data helps scientists understand the molecular make-up of ices on the surfaces of Pluto and Charon, as well as the age of geologic features such as craters. They can also tell us about surface changes caused by space “weather,” such as radiation. The new color images reveal that the “heart” of Pluto actually consists of two remarkably different-colored regions. In the false-color image, the heart consists of a western lobe shaped like an ice cream cone that appears peach color in this image. A mottled area on the right (east) side looks bluish. A mid-latitude band appears in shades ranging from pale blue through red. Even within the northern polar cap, in the upper part of the image, various shades of yellow-orange indicate subtle compositional differences. This image was obtained using three of the color filters of the Ralph instrument on July 13 at 3:38 am EDT and received on the ground on at 12:25 pm. Charon is Just as Colorful The surface of Charon is viewed using the same exaggerated color. The red on the dark northern polar cap of Charon is attributed to hydrocarbon and other molecules, a class of chemical compounds called tholins. The mottled colors at lower latitudes point to the diversity of terrains on Charon. This image was obtained using three of the color filters of the Ralph instrument on July 13 at 3:38 am EDT and received on the ground on at 12:25 pm. “We make these color images to highlight the variety of surface environments present in the Pluto system,” said Dennis Reuter, co-investigator with the New Horizons Composition Team. “They show us in an intuitive way that there is much still to learn from the data coming down.” Due to the three-billion-mile distance to Pluto, data takes 4 ½ hours to come to Earth, even at the speed of light. It will take 16 months for all of New Horizons’ science data to be received, and the treasure trove from this mission will be studied for decades to come. Image Caption: Pluto and Charon in False Color Show Compositional Diversity This July 13, 2015, image of Pluto and Charon is presented in false colors to make differences in surface material and features easy to see. It was obtained by the Ralph instrument on NASA's New Horizons spacecraft, using three filters to obtain color information, which is exaggerated in the image. These are not the actual colors of Pluto and Charon, and the apparent distance between the two bodies has been reduced for this side-by-side view. The image reveals that the bright heart-shaped region of Pluto includes areas that differ in color characteristics. The western lobe, shaped like an ice-cream cone, appears peach color in this image. A mottled area on the right (east) appears bluish. Even within Pluto's northern polar cap, in the upper part of the image, various shades of yellow-orange indicate subtle compositional differences. The surface of Charon is viewed using the same exaggerated color. The red on the dark northern polar cap of Charon is attributed to hydrocarbon materials including a class of chemical compounds called tholins. The mottled colors at lower latitudes point to the diversity of terrains on Charon. --- At 7:49 AM EDT on Tuesday, July 14 New Horizons sped past Pluto at 30,800 miles per hour (49,600 kilometers per hour), with a suite of seven science instruments. As planned, New Horizons went incommunicado as it hurtled through the Pluto-Charon system busily gathering data. The New Horizons team will breathe a sigh of relief when New Horizons “phones home” at approximately 9:02 p.m. EDT on July 14. The mission to the icy dwarf planet completes the initial reconnaissance of the solar system. Stay in touch with the New Horizons mission with #PlutoFlyby and on Facebook at: www.facebook.com/new.horizons1

The Frozen Canyons of Pluto North Pole

NASA Image and Video Library

2016-02-27

This ethereal scene captured by NASA New Horizons spacecraft tells yet another story of Pluto diversity of geological and compositional features-this time in an enhanced color image of the north polar area.

The Moons of Uranus, Neptune and Pluto.

ERIC Educational Resources Information Center

Brown, Robert Hamilton; Cruikshank, Dale P.

1985-01-01

In preparation for the Voyager flybys in 1989, the pace of ground-based investigations of the moons of Uranus, Neptune, and Pluto has quickened considerably. Information derived from these investigations is presented. (JN)

Alice Solar Occultation

NASA Image and Video Library

2015-07-17

This figure shows how the Alice instrument count rate changed over time during the sunset and sunrise observations. The count rate is largest when the line of sight to the sun is outside of the atmosphere at the start and end times. Molecular nitrogen (N2) starts absorbing sunlight in the upper reaches of Pluto's atmosphere, decreasing as the spacecraft approaches the planet's shadow. As the occultation progresses, atmospheric methane and hydrocarbons can also absorb the sunlight and further decrease the count rate. When the spacecraft is totally in Pluto's shadow the count rate goes to zero. As the spacecraft emerges from Pluto's shadow into sunrise, the process is reversed. By plotting the observed count rate in the reverse time direction, it is seen that the atmospheres on opposite sides of Pluto are nearly identical. http://photojournal.jpl.nasa.gov/catalog/PIA19716

Mapping Pluto Broken Heart

NASA Image and Video Library

2015-10-29

In addition to transmitting new high-resolution images and other data on the familiar close-approach hemispheres of Pluto and Charon, NASA's New Horizons spacecraft is also returning images -- such as this one -- to improve maps of other regions. This image was taken by the New Horizons Long Range Reconnaissance Imager (LORRI) on the morning of July 13, 2015, from a range of 1.03 million miles (1.7 million kilometers) and has a resolution of 5.1 miles (8.3 kilometers) per pixel. It provides fascinating new details to help the science team map the informally named Krun Macula (the prominent dark spot at the bottom of the image) and the complex terrain east and northeast of Pluto's "heart" (Tombaugh Regio). Pluto's north pole is on the planet's disk at the 12 o'clock position of this image. http://photojournal.jpl.nasa.gov/catalog/PIA20037

The small satellites of Pluto as observed by New Horizons.

PubMed

Weaver, H A; Buie, M W; Buratti, B J; Grundy, W M; Lauer, T R; Olkin, C B; Parker, A H; Porter, S B; Showalter, M R; Spencer, J R; Stern, S A; Verbiscer, A J; McKinnon, W B; Moore, J M; Robbins, S J; Schenk, P; Singer, K N; Barnouin, O S; Cheng, A F; Ernst, C M; Lisse, C M; Jennings, D E; Lunsford, A W; Reuter, D C; Hamilton, D P; Kaufmann, D E; Ennico, K; Young, L A; Beyer, R A; Binzel, R P; Bray, V J; Chaikin, A L; Cook, J C; Cruikshank, D P; Dalle Ore, C M; Earle, A M; Gladstone, G R; Howett, C J A; Linscott, I R; Nimmo, F; Parker, J Wm; Philippe, S; Protopapa, S; Reitsema, H J; Schmitt, B; Stryk, T; Summers, M E; Tsang, C C C; Throop, H H B; White, O L; Zangari, A M

2016-03-18

The New Horizons mission has provided resolved measurements of Pluto's moons Styx, Nix, Kerberos, and Hydra. All four are small, with equivalent spherical diameters of ~40 kilometers for Nix and Hydra and ~10 kilometers for Styx and Kerberos. They are also highly elongated, with maximum to minimum axis ratios of ~2. All four moons have high albedos (~50 to 90%) suggestive of a water-ice surface composition. Crater densities on Nix and Hydra imply surface ages of at least 4 billion years. The small moons rotate much faster than synchronous, with rotational poles clustered nearly orthogonal to the common pole directions of Pluto and Charon. These results reinforce the hypothesis that the small moons formed in the aftermath of a collision that produced the Pluto-Charon binary. Copyright © 2016, American Association for the Advancement of Science.

Heterogeneous and Evolving Distributions of Pluto's Volatile Surface Ices

NASA Astrophysics Data System (ADS)

Grundy, William M.; Olkin, C. B.; Young, L. A.; Buie, M. W.; Young, E. F.

2013-10-01

We report observations of Pluto's 0.8 to 2.4 µm reflectance spectrum with IRTF/SpeX on 70 nights over the 13 years from 2001 to 2013. The spectra show numerous vibrational absorption features of simple molecules CH4, CO, and N2 condensed as ices on Pluto's surface. These absorptions are modulated by the planet's 6.39 day rotation period, enabling us to constrain the longitudinal distributions of the three ices. Absorptions of CO and N2 are concentrated on Pluto's anti-Charon hemisphere, unlike absorptions of less volatile CH4 ice that are offset by roughly 90° from the longitude of maximum CO and N2 absorption. In addition to the diurnal/longitudinal variations, the spectra show longer term trends. On decadal timescales, Pluto's stronger CH4 absorption bands have deepened, while the amplitude of their diurnal variation has diminished, consistent with additional CH4 absorption by high northern latitude regions rotating into view as the sub-Earth latitude moves north (as defined by the system's angular momentum vector). Unlike the CH4 absorptions, Pluto's CO and N2 absorptions are declining over time, suggesting more equatorial or southerly distributions of those species. The authors gratefully thank the staff of IRTF for their tremendous assistance over the dozen+ years of this project. The work was funded in part by NSF grants AST-0407214 and AST-0085614 and NASA grants NAG5-4210 and NAG5-12516.

Soaring over Pluto

NASA Image and Video Library

2017-07-14

In July 2015, NASA's New Horizons spacecraft sent home the first close-up pictures of Pluto and its moons. Using actual New Horizons data and digital elevation models of Pluto and its largest moon, Charon, mission scientists created flyover movies that offer spectacular new perspectives of the many unusual features that were discovered and which have reshaped our views of the Pluto system -- from a vantage point even closer than a ride on New Horizons itself. The dramatic Pluto flyover begins over the highlands to the southwest of the great expanse of nitrogen ice plain informally named Sputnik Planitia. (Note that all feature names in the Pluto system are informal.) The viewer first passes over the western margin of Sputnik, where it borders the dark, cratered terrain of Cthulhu Macula, with the blocky mountain ranges located within the planitia seen on the right. The tour moves north past the rugged and fractured highlands of Voyager Terra and then turns southward over Pioneer Terra, which exhibits deep and wide pits, before concluding over the bladed terrain of Tartarus Dorsa in the far east of the encounter hemisphere. The topographic relief is exaggerated by a factor of 2 to 3 in these movies to emphasize topography; the surface colors have also been enhanced to bring out detail. Digital mapping and rendering were performed by Paul Schenk and John Blackwell of the Lunar and Planetary Institute in Houston. A video can be viewed at https://photojournal.jpl.nasa.gov/catalog/PIA21863

ON A GIANT IMPACT ORIGIN OF CHARON, NIX, AND HYDRA

DOE Office of Scientific and Technical Information (OSTI.GOV)

Canup, Robin M., E-mail: robin@boulder.swri.edu

It is generally believed that Charon was formed as a result of a large, grazing collision with Pluto that supplied the Pluto-Charon system with its high angular momentum. It has also been proposed that Pluto's small outer moons, Nix and Hydra, formed from debris from the Charon-forming impact, although the viability of this scenario remains unclear. Here I use smooth particle hydrodynamics impact simulations to show that it is possible to simultaneously form an intact Charon and an accompanying debris disk from a single impact. The successful cases involve colliding objects that are partially differentiated prior to impact, having thinmore » outer ice mantles overlying a uniform composition rock-ice core. The composition of the resulting debris disks varies from a mixture of rock and ice (similar to the bulk composition of Pluto and Charon) to a pure ice disk. If Nix and Hydra were formed from such an impact-generated disk, their densities should be less than or similar to that of Charon and Pluto, and the small moons could be composed entirely of ice. If they were instead formed from captured material, a mixed rock-ice composition and densities similar to that of Charon and Pluto would be expected. Improved constraints on the properties of Nix and Hydra through occultations and/or the New Horizons encounter may thus help to distinguish between these two modes of origin, particularly if the small moons are found to have ice-like densities.« less

Infrared spectoscopy of Triton and Pluto ice analogs: The case for saturated hydrocarbons

NASA Technical Reports Server (NTRS)

Bohn, Robert B.; Sandford, Scott A.; Allamandola, Louis J.; Cruikshank, Dale P.

1994-01-01

The infrared transmission spectra and photochemical behavior of various organic compounds isolated in solid N2 ices, appropriate for applications to Triton ad Pluto, are presented. It is shown that excess absorption in the surface spectra of Triton and Pluto, i.e., absorption not explained by present models incorporating molecules already identified on these bodies (N2, CH4, CO, and CO2), that starts near 4450/cm (2.25 microns) and extends to lower frequencies, may be due to alkanes (C(n)H(2n+2)) and related molecules frozen in the nitrogen. Branched and linear alkanes may be responsible. Experiments in which the photochemstry of N2: CH4 and N2: CH4: CO ices was explored demonsrtrate that the surface ices of Triton and Pluto may contain a wide variety of additional species containing H, C, O, and N. Of these, the reactive molecule diazomethane, CH2N2, is particularly important since it may be largely responsible for the synthesis of larger alkanes from CH4 and other small alkanes. Diazomethane would also be expected to drive chemical reactions involving organics in the surface ices of Triton and Pluto toward saturation, i.e., to reduce multiple CC bonds. The positions and intrinsic strengths (A values) of many of the infrared absorption bands of N2 matrix-isolated molecules of relevance to Triton and Pluto have also been determined. These can be used to aid in their search and to place constraints on their abundances.

Reorientation and faulting of Pluto due to volatile loading within Sputnik Planitia

NASA Astrophysics Data System (ADS)

Keane, James T.; Matsuyama, Isamu; Kamata, Shunichi; Steckloff, Jordan K.

2016-12-01

Pluto is an astoundingly diverse, geologically dynamic world. The dominant feature is Sputnik Planitia—a tear-drop-shaped topographic depression approximately 1,000 kilometres in diameter possibly representing an ancient impact basin. The interior of Sputnik Planitia is characterized by a smooth, craterless plain three to four kilometres beneath the surrounding rugged uplands, and represents the surface of a massive unit of actively convecting volatile ices (N2, CH4 and CO) several kilometres thick. This large feature is very near the Pluto-Charon tidal axis. Here we report that the location of Sputnik Planitia is the natural consequence of the sequestration of volatile ices within the basin and the resulting reorientation (true polar wander) of Pluto. Loading of volatile ices within a basin the size of Sputnik Planitia can substantially alter Pluto’s inertia tensor, resulting in a reorientation of the dwarf planet of around 60 degrees with respect to the rotational and tidal axes. The combination of this reorientation, loading and global expansion due to the freezing of a possible subsurface ocean generates stresses within the planet’s lithosphere, resulting in a global network of extensional faults that closely replicate the observed fault networks on Pluto. Sputnik Planitia probably formed northwest of its present location, and was loaded with volatiles over million-year timescales as a result of volatile transport cycles on Pluto. Pluto’s past, present and future orientation is controlled by feedbacks between volatile sublimation and condensation, changing insolation conditions and Pluto’s interior structure.

Pluto's Surface in Detail

NASA Image and Video Library

2017-07-14

On July 14, 2015, NASA's New Horizons spacecraft made its historic flight through the Pluto system. This detailed, high-quality global mosaic of Pluto was assembled from nearly all of the highest-resolution images obtained by the Long-Range Reconnaissance Imager (LORRI) and the Multispectral Visible Imaging Camera (MVIC) on New Horizons. The mosaic is the most detailed and comprehensive global view yet of Pluto's surface using New Horizons data. It includes topography data of the hemisphere visible to New Horizons during the spacecraft's closest approach. The topography is derived from digital stereo-image mapping tools that measure the parallax -- or the difference in the apparent relative positions -- of features on the surface obtained at different viewing angles during the encounter. Scientists use these parallax displacements of high and low terrain to estimate landform heights. The global mosaic has been overlain with transparent, colorized topography data wherever on the surface stereo data is available. Terrain south of about 30°S was in darkness leading up to and during the flyby, so is shown in black. Examples of large-scale topographic features on Pluto include the vast expanse of very flat, low-elevation nitrogen ice plains of Sputnik Planitia ("P") -- note that all feature names in the Pluto system are informal -- and, on the eastern edge of the encounter hemisphere, the aligned, high-elevation ridges of Tartarus Dorsa ("T") that host the enigmatic bladed terrain, mountains, possible cryovolcanos, canyons, craters and more. https://photojournal.jpl.nasa.gov/catalog/PIA21861

Pluto occultation on 2015 June 29 UTC with central flash and atmospheric spikes just before the New Horizons flyby

NASA Astrophysics Data System (ADS)

Pasachoff, Jay M.; Babcock, Bryce A.; Durst, Rebecca F.; Seeger, Christina H.; Levine, Stephen E.; Bosh, Amanda S.; Person, Michael J.; Sickafoose, Amanda A.; Zuluaga, Carlos A.; Kosiarek, Molly R.; Abe, Fumio; Nagakane, Masayuki; Suzuki, Daisuke; Tristram, Paul J.; Arredondo, Anicia

2017-11-01

We observed the occultation by Pluto of a 12th magnitude star, one of the two brightest occultation stars ever in our dozen years of continual monitoring of Pluto's atmosphere through such studies, on 2015 June 29 UTC. At the Univ. of Canterbury Mt. John Observatory (New Zealand), under clear skies throughout, we used a POETS frame-transfer CCD at 10 Hz with GPS timing on the 1-m McLellan telescope as well as an infrared camera on an 0.6-m telescope and three-color photometry at a slower cadence on a second 0.6-m telescope. At the Auckland Observatory, we used a POETS and a PICO on 0.5-m and 0.4-m telescopes, with 0.4 s and 2 s cadences, respectively, obtaining ingress observations before clouds moved in. The Mt. John light curves show a central flash, indicating that we were close to the center of the occultation path. Analysis of our light curves show that Pluto's atmosphere remains robust. The presence of spikes at both sites in the egress and ingress shows atmospheric layering. We coordinated our observations with aircraft observations (Bosh et al., 2017) with the Stratospheric Observatory for Infrared Astronomy (SOFIA). Our chords helped constrain the path across Pluto that SOFIA saw. Our ground-based and airborne stellar-occultation effort came only just over two weeks of Earth days and two Pluto days before the flyby of NASA's New Horizons spacecraft.

Risk of Contamination in Assembled vs Disassembled Instruments in Hip Arthroplasty Surgery.

PubMed

Mayer, Ryan R; Bederman, S Samuel; Colin, Vincent M; Berger, Martina M; Cesario, Thomas C; Schwarzkopf, Ran

2016-08-01

Periprosthetic joint infection (PJI) is one of the most common causes of revision total hip arthroplasty (THA) and associated with higher costs, prolonged pain, and worse clinical outcomes. Many factors have been linked to increased infection rates, one being the operative equipment and instrumentation used during the surgical procedure. With few arthroplasty instruments designed for complete disassembly and increasingly complex instrument designs, this study seeks to understand the effect that instrument disassembly plays on infection using disassembled and assembled standard femoral broach handles (BHs). Two BHs, not designed for disassembly, were modified and then contaminated in the disassembled state with Geobacillus stearothermophilus vegetative-form bacteria and spores. Using both flash and standard sterilization cycles, the BHs were steam sterilized in the disassembled or assembled state and then analyzed for remaining bacteria and spores. At all target locations after either a flash sterilization cycle or a standard sterilization cycle, complete eradication of both the vegetative-form and spore-form of G stearothermophilus was achieved. This study demonstrates that adequate decontamination of the tested BHs can be achieved after steam sterilization in either the disassembled or assembled state, without an increased risk of infection transmission. Copyright © 2016 Elsevier Inc. All rights reserved.

Risk of Contamination in Assembled vs Disassembled Instruments in Hip Arthroplasty Surgery

PubMed Central

Mayer, Ryan R.; Bederman, S. Samuel; Colin, Vincent M.; Berger, Martina M.; Cesario, Thomas C.; Schwarzkopf, Ran

2018-01-01

Background Periprosthetic joint infection (PJI) is one of the most common causes of revision total hip arthroplasty (THA) and associated with higher costs, prolonged pain, and worse clinical outcomes. Many factors have been linked to increased infection rates, one being the operative equipment and instrumentation used during the surgical procedure. With few arthroplasty instruments designed for complete disassembly and increasingly complex instrument designs, this study seeks to understand the effect that instrument disassembly plays on infection using disassembled and assembled standard femoral broach handles (BHs). Methods Two BHs, not designed for disassembly, were modified and then contaminated in the disassembled state with Geobacillus stearothermophilus vegetative-form bacteria and spores. Using both flash and standard sterilization cycles, the BHs were steam sterilized in the disassembled or assembled state and then analyzed for remaining bacteria and spores. Results At all target locations after either a flash sterilization cycle or a standard sterilization cycle, complete eradication of both the vegetative-form and spore-form of G stearothermophilus was achieved. Conclusion This study demonstrates that adequate decontamination of the tested BHs can be achieved after steam sterilization in either the disassembled or assembled state, without an increased risk of infection transmission. PMID:26948131

Latest Results from and Plans for the New Horizons Pluto-Kuiper Belt Mission

NASA Astrophysics Data System (ADS)

Weaver, Harold; Stern, Alan

2016-07-01

On 2015 July 14 NASA's New Horizons spacecraft flew 12,500 km above the surface of Pluto revealing a world of remarkable complexity and diversity. A giant basin filled with nitrogen ice dominated the encounter hemisphere and is the site of vigorous ongoing solid state convection that generates glacier-like transport along the surface. Giant mountains of water ice appear to be floating in the nitrogen ice. The periphery of the basin has a wide variety of landforms, including ice flow channels and chaotically arranged blocks of water ice. Extensive sublimation pitting is observed within the nitrogen ice sheet, testifying to active volatile transport. Peculiar bladed terrain to the east of the nitrogen ice sheet appears to be coated by methane ice. Pluto's equatorial region is dominated by an ancient dark red belt of material, probably tholins created either by irradiation of surface ices or by haze precipitation from the atmosphere. Pluto sports a wide variety of surface craters with some terrains dating back approximately 4 billion years while some terrains are geologically young. New Horizons discovered trace hydrocarbons in Pluto's atmosphere, multiple global haze layers, and a surface pressure near 10 microbars. Charon, Pluto's largest moon, displays tectonics, evidence for a heterogeneous crustal composition, and a puzzling giant hood of dark material covering its North Pole. Crater density statistics for Charon's surface give a crater retention age of 4-4.5 Ga, indicating that Charon's geological evolution largely ceased early in its history. All of Pluto's four small moons (Styx, Nix, Kerberos, and Hydra) have high albedos, highly elongated shapes, and are rotating much faster then synchronous with their orbital periods, with rotational poles clustered near the Pluto-Charon orbital plane. The surfaces of Nix and Hydra are coated with nearly pristine crystalline water ice, despite having crater retention ages greater than 4 billion years. The New Horizons spacecraft remains healthy and was targeted toward the flyby of a small (~30-40 km) KBO in late-2015, enabling the study of an object (2014 MU69) in a completely different dynamical class (cold classical) than Pluto, if NASA approves an Extended Mission phase. In addition to the flyby of 2014 MU69 on 2019-Jan-01, the proposed Extended Mission would also include observations of more than 20 other KBOs at resolutions and geometries not feasible from Earth, and studies of the heliospheric plasma, neutral H and He, and the dust environment out to 50 AU from the Sun.

Influence of Bulk Carbonaceous Matter on Pluto's Structure and Evolution

NASA Astrophysics Data System (ADS)

McKinnon, W. B.; Stern, S. A.; Weaver, H. A., Jr.; Spencer, J. R.; Moore, J. M.; Young, L. A.; Olkin, C.

2017-12-01

The rock/ice mass ratio of the Pluto system is about 2/1 (McKinnon et al., Icarus 287, 2017) [1], though this neglects the potential role of bulk carbonaceous matter ("CHON"), an important cometary component and one likely important in the ancestral Kuiper belt. The wealth of measurements at comet 67P/Churyumov-Gerasimenko (a Jupiter-family comet and thus one formed in the same region of the outer Solar System as Pluto) by Rosetta are particularly instructive. E.g., Davidsson et al. (A&A 592, 2016) [2] propose in their "composition A" that 67P/Ch-G is 25% metal/sulfides, 42% rock/organics, and 32% ice by mass. For their assumed component densities, the overall grain density is 1820 kg/m3. Fulle et al. (MNRAS 462, 2016) [3] posit 5 ± 2 volume % Fe-sulfides of density 4600 kg/m3, 28 ± 5% Mg,Fe-olivines and -pyroxenes of density 3200 kg/m3, 52 ± 12% hydrocarbons of density 1200 kg/m3, and 15 ± 6% ices of 917 kg/m3. This composition yields a primordial grain density (dust + ice) of 1885 ± 240 kg/m3. Both of these cometary density estimates [2,3] are consistent with Pluto-Charon, especially as Pluto's uncompressed (STP) density is close to 1820 kg/m3 and that of the system as a whole is close to 1800 kg/m3 [1]. We consider the potential compositional and structural implications of these proposed 67P/Ch-G compositions when applied to Pluto and Charon. The amount of ice in model A of [2] is a good match to Pluto structural models. Their rock/organics component, however, is taken to be half graphite (2000 kg/m3) by volume. The composition in [3] is more divergent: very ice poor, and on the order of 50% light hydrocarbons by volume. Regardless of the differences between [2] and [3], the possibility of massive internal graphite or carbonaceous layers within Pluto is real. We discuss the possible consequences for Pluto's structure, rock/ice ratio, thermal and chemical evolution, and even interpretation of its gravity field from tectonics. For example, radiogenic heat flows could be lessened in comparison with pure ice+rock±ocean interior models. And could the inferred gravity high at Sputnik Planitia (Nimmo et al., Nature 540, 2016) actually be due to an uplifted graphite-rich layer? A bulk carbonaceous contribution to icy satellites is also possible, and may behind the rich organic chemistry in Enceladus' plume vapor (Waite et al., Nature 460, 2009).

The New Horizons and Hubble Space Telescope search for rings, dust, and debris in the Pluto-Charon system

NASA Astrophysics Data System (ADS)

Lauer, Tod R.; Throop, Henry B.; Showalter, Mark R.; Weaver, Harold A.; Stern, S. Alan; Spencer, John R.; Buie, Marc W.; Hamilton, Douglas P.; Porter, Simon B.; Verbiscer, Anne J.; Young, Leslie A.; Olkin, Cathy B.; Ennico, Kimberly; New Horizons Science Team

2018-02-01

We conducted an extensive search for dust or debris rings in the Pluto-Charon system before, during, and after the New Horizons encounter in July 2015. Methodologies included attempting to detect features by back-scattered light during the approach to Pluto (phase angle α ∼ 15°), in situ detection of impacting particles, a search for stellar occultations near the time of closest approach, and by forward-scattered light imaging during departure (α ∼ 165°). An extensive search using the Hubble Space Telescope (HST) prior to the encounter also contributed to the final ring limits. No rings, debris, or dust features were observed, but our new detection limits provide a substantially improved picture of the environment throughout the Pluto-Charon system. Searches for rings in back-scattered light covered the range 35,000-250,000 km from the system barycenter, a zone that starts interior to the orbit of Styx, the innermost minor satellite, and extends out to four times the orbital radius of Hydra, the outermost known satellite. We obtained our firmest limits using data from the New Horizons LORRI camera in the inner half of this region. Our limits on the normal I/F of an unseen ring depends on the radial scale of the rings: 2 ×10-8 (3σ) for 1500 km wide rings, 1 ×10-8 for 6000 km rings, and 7 ×10-9 for 12,000 km rings. Beyond ∼ 100, 000 km from Pluto, HST observations limit normal I/F to ∼ 8 ×10-8 . Searches for dust features from forward-scattered light extended from the surface of Pluto to the Pluto-Charon Hill sphere (rHill = 6.4 ×106 km). No evidence for rings or dust clouds was detected to normal I/F limits of ∼ 8.9 ×10-7 on ∼ 104 km scales. Four stellar occulation observations also probed the space interior to Hydra, but again no dust or debris was detected. The Student Dust Counter detected one particle impact 3.6 × 106 km from Pluto, but this is consistent with the interplanetary space environment established during the cruise of New Horizons. Elsewhere in the solar system, small moons commonly share their orbits with faint dust rings. Our results support recent dynamical studies suggesting that small grains are quickly lost from the Pluto-Charon system due to solar radiation pressure, whereas larger particles are orbitally unstable due to ongoing perturbations by the known moons.

Volatile Transport Implications from the New Horizons Flyby of Pluto

NASA Astrophysics Data System (ADS)

Young, Leslie; Grundy, William M.; Binzel, RIchard P.; Earle, Alissa M.; Linscott, Ivan R.; Hinson, David P.; Zangari, Amanda M.; McKinnon, William B.; Stern, S. Alan; Weaver, Harold A.; Olkin, Catherine B.; Ennico, Kimberly; Gladstone, G. Randall; Summers, Michael E.; Moore, Jeffrey M.; Spencer, John R.

2015-11-01

The New Horizons flyby of Pluto has revealed a striking range of terrains, from the very bright region informally named Sputnik Planum, to very dark regions such as the informally named Cthulhu Regio. Such a variety was beyond the scope of recent models of Pluto's seasonal volatile cycle (Young 2013, ApJL 766, L22; Hansen, Paige and Young 2015, Icarus 246, 183), which assumed globally uniform substrate albedos. The "Exchange with Pressure Plateau (EPP)" class of models in Young (2013) and the favored runs from Hansen et al (2015) had long periods of exchange of volatiles between northern and southern hemispheres. In these models, the equators were largely devoid of volatiles; even though the equatorial latitudes received less insolation than the poles over a Pluto year, they were never the coldest place on the icy world. New models that include a variety of substrate albedos can investigate questions such as whether Sputnik Planum has an albedo that is high enough to act as a local cold trap for much of Pluto's year. We will present the implications of this and other assumption-busting revelations from the New Horizons flyby. This work was supported by NASA’s New Horizons project.

Albedo matters: Understanding runaway albedo variations on Pluto

NASA Astrophysics Data System (ADS)

Earle, Alissa M.; Binzel, Richard P.; Young, Leslie A.; Stern, S. A.; Ennico, K.; Grundy, W.; Olkin, C. B.; Weaver, H. A.; New Horizons Surface Composition Theme

2018-03-01

The data returned from NASA's New Horizons reconnaissance of the Pluto system show striking albedo variations from polar to equatorial latitudes as well as sharp longitudinal boundaries. Pluto has a high obliquity (currently 119°) that varies by 23° over a period of less than 3 million years. This variation, combined with its regressing longitude of perihelion (360° over 3.7 million years), creates epochs of "Super Seasons" where one pole is pointed at the Sun at perihelion, thereby experiencing a short, relatively warm summer followed by its longest possible period of winter darkness. In contrast, the other pole experiences a much longer, less intense summer and a short winter season. We use a simple volatile sublimation and deposition model to explore the relationship between albedo variations, latitude, and volatile sublimation and deposition for the current epoch as well as historical epochs during which Pluto experienced these "Super Seasons." Our investigation quantitatively shows that Pluto's geometry creates the potential for runaway albedo and volatile variations, particularly in the equatorial region, which can sustain stark longitudinal contrasts like the ones we see between Tombaugh Regio and the informally named Cthulhu Regio.

In search of a signature of binary Kuiper Belt Objects in the Pluto-Charon crater population

NASA Astrophysics Data System (ADS)

Zangari, Amanda Marie; Parker, Alex; Singer, Kelsi N.; Stern, S. Alan; Young, Leslie; Olkin, Catherine B.; Ennico, Kimberly; Weaver, Harold A.; New Horizons Geology, Geophysics and Imaging Science Theme Team

2016-10-01

In July 2015, New Horizons flew by Pluto and Charon, allowing mapping of the encounter hemisphere at high enough resolution to produce crater counts from the surfaces of the pair. We investigate the distribution of craters in search of a signature of binary impactors. The Kuiper Belt -- especially the cold classical region -- has a large fraction of binary objects, many of which are close-in, equal-mass binaries. We will present results on how the distribution of craters seen on Pluto and Charon compares to a random distribution of single body impactors on the surfaces of each. Examining the surfaces of Pluto and Charon proves challenging due to resurfacing, and the presence of tectonic and other geographic features. For example, the informally-named Cthulhu region is among the oldest on Pluto, yet it abuts a craterless region millions of years young. On Charon, chastmata divide the surface into regions informally named Vulcan Planum and Oz terra. In our statistics, we pay careful attention to the boundaries of where craters may appear, and the dependence of our results on crater size. This work was supported by NASA's New Horizons project.

New Horizons Best Close-Up of Pluto Surface

NASA Image and Video Library

2016-05-27

This mosaic strip, extending across the hemisphere that faced the New Horizons spacecraft as it flew past Pluto on July 14, 2015, now includes all of the highest-resolution images taken by the NASA probe.

Geological Mapping of the Encounter Hemisphere on Pluto

NASA Astrophysics Data System (ADS)

White, O. L.; Moore, J. M.; Stern, S. A.; Weaver, H. A.; Olkin, C. B.; Ennico, K.; Young, L. A.; Cheng, A. F.; New Horizons GGI Theme Team

2016-06-01

We present mapping of Pluto's encounter hemisphere performed to date (focusing on Sputnik Planum and the immediately surrounding area) and offer preliminary descriptions of terrains further afield that will be the subject of future mapping.

Into the Kuiper Belt: New Horizons Post-Pluto

NASA Astrophysics Data System (ADS)

Harrison Parker, Alex; Spencer, John; Benecchi, Susan; Binzel, Richard; Borncamp, David; Buie, Marc; Fuentes, Cesar; Gwyn, Stephen; Kavelaars, JJ; Noll, Keith; Petit, Jean-Marc; Porter, Simon; Showalter, Mark; Stern, S. Alan; Sterner, Ray; Tholen, David; Verbiscer, Anne; Weaver, Hal; Zangari, Amanda

2015-11-01

New Horizons is now beyond Pluto and flying deeper into the Kuiper Belt. In the summer of 2014, a Hubble Space Telescope Large Program identified two candidate Cold Classical Kuiper Belt Objects (KBOs) that were within reach of New Horizons' remaining fuel budget. Here we present the selection of the Kuiper Belt flyby target for New Horizons' post-Pluto mission, our state of knowledge regarding this target and the potential 2019 flyby, the status of New Horizons' targeting maneuver, and prospects for near-future long-range observations of other KBOs.

Observational constraint on Pluto's atmospheric CO with ASTE

NASA Astrophysics Data System (ADS)

Iino, Takahiro; Hirahara, Yasuhiro; Hidemori, Takehiro; Tsukagoshi, Takashi; Nakajima, Taku; Nakamoto, Satoru; Kato, Chihaya

2016-02-01

To confirm the previous observational results of Pluto's atmospheric CO in the J = 2-1 rotational transition, we conducted a new observation of CO (J = 3-2) in Pluto's atmosphere in 2014 August with the Atacama Submillimeter Telescope Experiment 10 m single-dish telescope. In contrast to the previous observational result obtained with the James Clerk Maxwell Telescope in 2009 and 2010 by using the J = 2-1 transition, no emission structure was observed near the rest frequency in our attempt. Possible explanations for the nondetection result of the J = 3-2 transition are discussed.

Pluto Moon Nix, Half Illuminated

NASA Image and Video Library

2015-12-18

This recently received panchromatic image of Pluto's small satellite Nix taken by the Multispectral Visible Imaging Camera (MVIC) aboard New Horizons is one of the best images of Pluto's third-largest moon generated by the NASA mission. Taken on July 14, 2015, at a range of about 14,000 miles (23,000 kilometers) from Nix, the illuminated surface is about 12 miles (19 kilometers) by 29 miles (47 kilometers). The unique perspective of this image provides new details about Nix's geologic history and impact record. http://photojournal.jpl.nasa.gov/catalog/PIA20287

Partly Cloudy on Pluto?

NASA Image and Video Library

2016-10-18

Pluto's present, hazy atmosphere is almost entirely free of clouds, though scientists from NASA's New Horizons mission have identified some cloud candidates after examining images taken by the New Horizons Long Range Reconnaissance Imager and Multispectral Visible Imaging Camera, during the spacecraft's July 2015 flight through the Pluto system. All are low-lying, isolated small features -- no broad cloud decks or fields -- and while none of the features can be confirmed with stereo imaging, scientists say they are suggestive of possible, rare condensation clouds. http://photojournal.jpl.nasa.gov/catalog/PIA21127

The First U.S. Naval Observatory Robotic Astrometric Telescope Catalog

DTIC Science & Technology

2015-10-01

in the “info” folder. URAT1 covers almost the entire northern sky and most of the area δ �−15°, plus the far south area around Pluto . 2.3. Robotic...meeting acceptable quality standards. A total of 14 and 12 exposures of the Pluto field area taken on 2013 September 19 and 2014 September 06...for our project. 2MASS was used for near-IR photometry and as the first epoch of URAT1 proper motions. Bill Gray (Project Pluto ) is thanked for making

Mapping Pluto Methane Ice

NASA Image and Video Library

2015-09-24

The Ralph/LEISA infrared spectrometer on NASA's New Horizons spacecraft mapped compositions across Pluto's surface as it flew past the planet on July 14, 2015. On the left, a map of methane ice abundance shows striking regional differences, with stronger methane absorption indicated by the brighter purple colors, and lower abundances shown in black. Data have only been received so far for the left half of Pluto's disk. At right, the methane map is merged with higher-resolution images from the spacecraft's Long Range Reconnaissance Imager (LORRI). http://photojournal.jpl.nasa.gov/catalog/PIA19953

Surface ices and the atmospheric composition of Pluto

NASA Technical Reports Server (NTRS)

Owen, Tobias C.; Roush, Ted L.; Cruikshank, Dale P.; Elliot, James L.; Young, Leslie A.; De Bergh, Catherine; Schmitt, Bernard; Geballe, Thomas R.; Brown, Robert H.; Bartholomew, Mary J.

1993-01-01

Observations of the 1.4- to 2.4-micrometer spectrum of Pluto reveal absorptions of carbon monoxide and nitrogen ices and confirm the presence of solid methane. Frozen nitrogen is more abundant than the other two ices by a factor of about 50; gaseous nitrogen must therefore be the major atmospheric constituent. The absence of carbon dioxide absorptions is one of several differences between the spectra of Pluto and Triton in this region. Both worlds carry information about the composition of the solar nebula and the processes by which icy planetesimals formed.

The Chemistry of Pluto and its Satellites

NASA Technical Reports Server (NTRS)

Cruikshank, Dale P.

2017-01-01

Pluto's bulk composition and the composition of the surface layers hold clues to the origin and evolution of a number of other Solar System bodies of comparable size in the region beyond Neptune. The July 14, 2015 flyby of the Pluto system with the New Horizons spacecraft afforded the opportunity to corroborate and greatly improve discoveries about the planet and its satellites derived Earth-based studies. It also revealed extraordinary details of the surface and atmosphere of Pluto, as well as the geology and composition of Charon and two smaller satellites. With a mean density of 1.86 g/sq cm, the bulk composition of Pluto is about two-thirds anhydrous solar composition rocky material and one-third volatiles (primarily H2O in liquid and solid states) by mass, the surface is a veneer of ices dominated by N2, with smaller amounts of CH4 and CO, as well as limited exposures of H2O ice (considered to be "bedrock"). N2, CH4, and CO occur as solid solutions at temperature-dependent mutual concentrations, each component being soluble in the others. Frozen C2H6 as a minor component has also been identified. Sublimation and recondensation of N2, CH4, and CO over seasonal (248 y) and Milankovich-type megaseasons (approx. 3 My) result in the redistribution of these ices over time and with latitude control. Solid N2 is found in glaciers originating in higher elevations and flowing at the present time into a basin structure larger than the State of Texas, forming a convecting lens of N2 that overturns on a timescale of order 10 My. The varied colors of Pluto's landscape arise from the energetic processing of the surface ices in processes that break the simple molecules and reassemble complex organic structures consisting of groups of aromatic rings connected by aliphatic chains. When synthesized in the laboratory by UV or electron irradiation of a Pluto mix of ice, this material, called tholin, has colors closely similar to Pluto. The Pluto ice tholin analog contains carboxylic acids, urea, ketones, aldehydes, amines, and some nitriles. The largest satellite, Charon has density 1.70 g/sq cm and it is about 3/5 anhydrous solar composition rock, with the remainder in H2O ice. The surface H2O ice is infused in some way with NH3, probably as a hydrate, distributed nonuniformly, but to some degree related to geological structures. Pluto's atmosphere is N2, CH4, with CO, C2-hydrocarbons, HCN, and other molecules in trace but detectable amounts. The atmosphere supports a complex haze structure with about 20 discrete layers, and suspected clouds. The haze is presumed to be made of aggregates of complex hydrocarbons (tholins) produced by photolysis of the atmospheric gases, and with similar composition to the ice tholins made on the planet's surface. Urea and a suite of carboxylic acids are of interest for prebiotic and biological chemistries.

A Search for Temporal Changes on Pluto and Charon

NASA Astrophysics Data System (ADS)

Hofgartner, Jason D.; Buratti, Bonnie J.; Devins, Spencer; Beyer, Ross A.; Schenk, Paul M.; Stern, S. Alan; Weaver, Harold A.; Olkin, Catherine; Cheng, Andrew F.; Ennico, Kimberly; Lauer, Tod R.; Spencer, John R.; Young, Leslie; New Horizons Science Team

2017-10-01

A search for temporal changes on Pluto and Charon was motivated by (1) the discovery of young surfaces in the Pluto system that imply ongoing or recent geologic activity, (2) the detection of active plumes on Triton during the Voyager 2 flyby, and (3) the abundant and detailed information that observing geologic processes in action provides about the processes. A thorough search for temporal changes using New Horizons images was completed. Images that covered the same region were blinked and manually inspected for any differences in appearance. The search included full-disk images such that all illuminated regions of both bodies were investigated and also higher resolution images such that parts of the encounter hemispheres were investigated at finer spatial scales. Changes of appearance between different images were observed but in all cases were attributed to variability of the imaging parameters (especially geometry) or artifacts. No differences of appearance that are strongly indicative of a temporal change were found on the surface or in the atmosphere of either Pluto or Charon. Limits on temporal changes as a function of spatial scale and temporal interval during the New Horizons encounter are determined. The longest time interval constraint is one Pluto/Charon rotation period (~6.4 Earth days). Contrast reversal and high-phase bright features that change in appearance with solar phase angle are identified. The change of appearance of these features is most likely due to the change in phase angle rather than a temporal change. Had active plumes analogous to the plumes discovered on Triton been present on the encounter hemispheres of either Pluto or Charon, they would have been detected. Several dark streak features that may be deposits from past plumes are identified. The absence of active plumes may be due to temporal variability or because the process that generates Triton’s plumes does not occur on Pluto.

Discovery Orbiter Major Modifications

NASA Image and Video Library

2003-08-27

During power-up of the orbiter Discovery in the Orbiter Processing Facility, a technician moves a circuit reset on the cockpit console. Discovery has been undergoing Orbiter Major Modifications in the past year, ranging from wiring, control panels and black boxes to gaseous and fluid systems tubing and components. These systems were deserviced, disassembled, inspected, modified, reassembled, checked out and reserviced, as were most other systems onboard. The work includes the installation of the Multifunction Electronic Display Subsystem (MEDS) - a state-of-the-art “glass cockpit.”

Low cytoplasmic pH reduces ER-Golgi trafficking and induces disassembly of the Golgi apparatus.

PubMed

Soonthornsit, Jeerawat; Yamaguchi, Yoko; Tamura, Daisuke; Ishida, Ryuichi; Nakakoji, Yoko; Osako, Shiho; Yamamoto, Akitsugu; Nakamura, Nobuhiro

2014-11-01

The Golgi apparatus was dramatically disassembled when cells were incubated in a low pH medium. The cis-Golgi disassembled quickly, extended tubules and spread to the periphery of cells within 30 min. In contrast, medial- and trans-Golgi were fragmented in significantly larger structures of smaller numbers at a slower rate and remained largely in structures distinct from the cis-Golgi. Electron microscopy revealed the complete disassembly of the Golgi stack in low pH treated cells. The effect of low pH was reversible; the Golgi apparatus reassembled to form a normal ribbon-like structure within 1-2h after the addition of a control medium. The anterograde ER to Golgi transport and retrograde Golgi to ER transport were both reduced under low pH. Phospholipase A2 inhibitors (ONO, BEL) effectively suppressed the Golgi disassembly, suggesting that the phospholipase A2 was involved in the Golgi disassembly. Over-expression of Rab1, 2, 30, 33 and 41 also suppressed the Golgi disassembly under low pH, suggesting that they have protective role against Golgi disassembly. Low pH treatment reduced cytoplasmic pH, but not the luminal pH of the Golgi apparatus, strongly suggesting that reduction of the cytoplasmic pH triggered the Golgi disassembly. Because a lower cytoplasmic pH is induced in physiological or pathological conditions, disassembly of the Golgi apparatus and reduction of vesicular transport through the Golgi apparatus may play important roles in cell physiology and pathology. Furthermore, our findings indicated that low pH treatment can serve as an important tool to analyze the molecular mechanisms that support the structure and function of the Golgi apparatus. Copyright © 2014 Elsevier Inc. All rights reserved.

Two Faces of Pluto July 1

NASA Image and Video Library

2015-12-31

Pluto shows two remarkably different sides in these color images of the planet and its largest moon, Charon, taken by NASA New Horizons on June 25 and June 27, 2015. http://photojournal.jpl.nasa.gov/catalog/PIA20292

Planetary science: Pluto's polygons explained

NASA Astrophysics Data System (ADS)

Dombard, Andrew J.; O'Hara, Sean

2016-06-01

The Sputnik Planum basin of Pluto contains a sheet of nitrogen ice, the surface of which is divided into irregular polygons tens of kilometres across. Two studies reveal that vigorous convection causes these polygons. See Letters p.79 & 82

The Atmospheres of Pluto and Charon

NASA Astrophysics Data System (ADS)

Gladstone, R.; Summers, M. E.; Stern, A.; Ennico Smith, K.; Olkin, C.; Weaver, H. A., Jr.; Young, L. A.; Strobel, D. F.; Hinson, D. P.; Kammer, J.; Parker, A. H.; Steffl, A.; Linscott, I.; Parker, J. W.; Cheng, A. F.; Versteeg, M. H.; Greathouse, T.; Retherford, K. D.; Throop, H.; Woods, W. W.; Singer, K. N.; Tsang, C.; Schindhelm, E.; Wong, M. L.; Yung, Y. L.; Zhu, X.; Curdt, W.; Lavvas, P.; Young, E. F.; Tyler, G. L.

2015-12-01

Major goals of the New Horizons (NH) mission are to explore and characterize the structure and composition of Pluto's atmosphere, and to determine whether Charon has a measurable atmosphere of its own. Several instruments onboard NH contribute to these goals, primarily: 1) the REX instrument, through uplink X-band radio occultations, 2) the Alice instrument, through extreme- and far-ultraviolet solar occultations, and 3) the LORRI panchromatic imager, through high-phase-angle imaging. The associated datasets were obtained following closest approach of NH to Pluto. Pressure and temperature profiles of the lower atmosphere are derived from the REX data, the composition and structure of the extended atmosphere are derived from the Alice data (supported by approach observations of reflected ultraviolet sunlight), and the distribution and properties of Pluto's hazes are derived from the LORRI data. In this talk an overview of the early atmosphere science results will be presented.

A Heart on Pluto

NASA Image and Video Library

2015-07-08

In the early morning hours of July 8, 2015, mission scientists received this new view of Pluto -- the most detailed yet returned by the Long Range Reconnaissance Imager (LORRI) aboard New Horizons. The image was taken on July 7, when the NASA spacecraft was just under 5 million miles (8 million kilometers) from Pluto, and is the first to be received since the July 4 anomaly that sent the spacecraft into safe mode. This view is centered roughly on the area that will be seen close-up during New Horizons' July 14 closest approach. This side of Pluto is dominated by three broad regions of varying brightness. Most prominent are an elongated dark feature at the equator, informally known as "the whale," and a large heart-shaped bright area measuring some 1,200 miles (2,000 kilometers) across on the right. Above those features is a polar region that is intermediate in brightness. http://photojournal.jpl.nasa.gov/catalog/PIA19702

Recent tectonic activity on Pluto driven by phase changes in the ice shell

NASA Astrophysics Data System (ADS)

Hammond, Noah P.; Barr, Amy C.; Parmentier, Edgar M.

2016-07-01

The New Horizons spacecraft has found evidence for geologic activity on the surface of Pluto, including extensional tectonic deformation of its water ice bedrock see Moore et al. (2016). One mechanism that could drive extensional tectonic activity is global surface expansion due to the partial freezing of an ocean. We use updated physical properties for Pluto and simulate its thermal evolution to understand the survival of a possible subsurface ocean. For thermal conductivities of rock less than 3 W m-1 K-1, an ocean forms and at least partially freezes, leading to recent extensional stresses in the ice shell. In scenarios where the ocean freezes and the ice shell is thicker than 260 km, ice II forms and causes global volume contraction. Since there is no evidence for recent compressional tectonic features, we argue that ice II has not formed and that Pluto's ocean has likely survived to present day.

Small Bodies in the Kuiper Belt : Lessons from Pluto's Small Satellites

NASA Astrophysics Data System (ADS)

Weaver, H. A., Jr.; Buie, M. W.; Howett, C.; Olkin, C.; Parker, A. H.; Parker, J. W.; Porter, S. B.; Robbins, S. J.; Singer, K. N.; Spencer, J. R.; Stern, A.; Young, L. A.; Zangari, A. M.; Lauer, T.; Showalter, M.; Verbiscer, A.; McKinnon, W. B.; Cook, J. C.; Grundy, W. M.; Protopapa, S.; Hamilton, D. P.; Schmitt, B.; Buratti, B. J.; Binzel, R. P.; Jennings, D. E.; Reuter, D.; Cruikshank, D. P.; Dalle Ore, C.; Ennico Smith, K.; Moore, J. M.; Cheng, A. F.; Lisse, C. M.

2017-12-01

During the approach and flyby of the Pluto system in 2015, the instruments on theNew Horizons spacecraft obtained data on Pluto's small satellites that far surpassedwhat was previously available. All four small moons (Styx, Nix, Kerberos, and Hydra,in order of distance from Pluto) have highly irregular shapes, rapid non-synchronous rotation rates, high obliquity rotational poles, high visible albedos ( 50-80%), andneutral-to-blue visible colors. The even more detailed information obtained for Nix and Hydra reveal those 40 km diameter objects to have relatively ancient ( 3-4 Gyr) surfacesdominated by crystalline water ice, but with a hint of ammonia-containing compounds. Here we addresswhat these results say about the origin and evolution of these bodies, and howthese results inform studies of other small bodies in the Kuiper belt, including2014 MU69, the next flyby target for the New Horizons mission.

Comparative Proteomics Reveals Timely Transport into Cilia of Regulators or Effectors as a Mechanism Underlying Ciliary Disassembly.

PubMed

Wang, Limei; Gu, Lixiao; Meng, Dan; Wu, Qiong; Deng, Haiteng; Pan, Junmin

2017-07-07

Primary cilia are assembled and disassembled during cell cycle progression. During ciliary disassembly, ciliary axonemal microtubules (MTs) are depolymerized accompanied by extensive posttranslational protein modifications of ciliary proteins including protein phosphorylation, methylation, and ubiquitination. These events are hypothesized to involve transport of effectors or regulators into cilia at the time of ciliary disassembly from the cell body. To prove this hypothesis and identify new proteins involved in ciliary disassembly, we analyzed disassembling flagella in Chlamydomonas using comparative proteomics with TMT labeling. Ninety-one proteins were found to increase more than 1.4-fold in four replicates. The proteins of the IFT machinery not only increase but also exhibit stoichiometric changes. The other proteins that increase include signaling molecules, chaperones, and proteins involved in microtubule dynamics or stability. In particular, we have identified a ciliopathy protein C21orf2, the AAA-ATPase CDC48, that is involved in segregating polypeptides from large assemblies or cellular structures, FAP203 and FAP236, which are homologous to stabilizers of axonemal microtubules. Our data demonstrate that ciliary transport of effectors or regulators is one of the mechanisms underlying ciliary disassembly. Further characterization of the proteins identified will provide new insights into our understanding of ciliary disassembly and likely ciliopathy.

Exploring potential Pluto-generated neutral tori

NASA Astrophysics Data System (ADS)

Smith, Howard T.; Hill, Matthew; KollMann, Peter; McHutt, Ralph

2015-11-01

The NASA New Horizons mission to Pluto is providing unprecedented insight into this mysterious outer solar system body. Escaping molecular nitrogen is of particular interest and possibly analogous to similar features observed at moons of Saturn and Jupiter. Such escaping N2 has the potential of creating molecular nitrogen and N (as a result of molecular dissociation) tori or partial toroidal extended particle distributions. The presence of these features would present the first confirmation of an extended toroidal neutral feature on a planetary scale in our solar system. While escape velocities are anticipated to be lower than those at Enceladus, Io or even Europa, particle lifetimes are much longer in Pluto’s orbit because as a result of much weaker solar interaction processes along Pluto’s orbit (on the order of tens of years). Thus, with a ~248 year orbit, Pluto may in fact be generating an extended toroidal feature along it orbit.For this work, we modify and apply our 3-D Monte Carlo neutral torus model (previously used at Saturn, Jupiter and Mercury) to study/analyze the theoretical possibility and scope of potential Pluto-generated neutral tori. Our model injects weighted particles and tracks their trajectories under the influence of all gravitational fields with interactions with other particles, solar photons and Pluto collisions. We present anticipated N2 and N tori based on current estimates of source characterization and environmental conditions. We also present an analysis of sensitivity to assumed initial conditions. Such results can provide insight into the Pluto system as well as valuable interpretation of New Horizon’s observational data.

(abstract) Follow-on Missions for the Pluto Spacecraft

NASA Technical Reports Server (NTRS)

Weinstein, Stacy; Salvo, Chris; Stern, Alan

1994-01-01

The Pluto Fast Flyby mission development baseline consists of 2 identical spacecraft (120 - 165 kg) to be launched to Pluto/Charon in the late 1990s. These spacecraft are intended to fly by Pluto and Charon in order to perform various remote-sensing scientific investigations and have a mission development cost less than $400M (FY92$) through launch plus 30 days. The long-life (6 - 10 years) mission duration and lightweight design make the Pluto spacecraft a good candidate for a number of other flyby missions to objects in the outer Solar System, and some of these were investigated by JPL in cooperation with NASA Code SL's (Solar System Exploration) Outer Planets Science Working Group (OPSWG) in 1993. The JPL team looked at what it would mean to fly one of these missions (if a third spacecraft were available) in terms of flight time, spacecraft modifications, and science payload resources; the OPSWG recommended science investigation modifications for the different targets based on the available resources. The missions could, in many cases, utilize less capable launch vehicles, thereby reducing life-cycle cost of the mission. Examples of the sort of targets which were investigated and looked attractive in terms of flight time are: Uranus, Neptune, Uranus/Neptune dual-mission, Trojan asteroids (624 Hektor, 617 Patroclus, others), 5145 Pholus (the reddest object known in the solar system), and Kuiper Belt objects (i.e., 1992 QB1) . This paper will present the results of this investigation in terms of potential science return, performance, and the potential for life-cycle cost reductions through inheritance from Pluto Fast Flyby .

Analysis of Archival Low-Resolution Near-Infrared Spectra to Measure Pluto's Atmosphere.

NASA Astrophysics Data System (ADS)

Cook, Jason C.; Young, Leslie; Cruikshank, Dale P.

2017-10-01

First detected via occultation observations, Pluto's atmosphere has changed since its discovery in the 1980s (Brosch & Mendelson, 1985; Elliot et al., 1989). Between the occultations of 1988 and 2002, the surface pressure doubled (Elliot et al., 2003) as Pluto passed through perihelion in 1989. In the years following the 2002 occultation, only a slight increase in the surface pressure has been noted (Young et al. 2013; Olkin et al. 2015). High-resolution spectroscopy has also been used to determine the composition of Pluto's atmosphere. This was first successfully done in 1992 (Young et al., 1997), but no follow up detection was made until 2008 (Lellouch et al. 2009). With a gap in the occultation and spectroscopic records, we have little information on how and when Pluto's atmosphere changed. In order to fill in this gap, we are examining low spectral resolution, high signal-to-noise spectra of Pluto such as Cook et al (2014) presented previously. At this meeting, we will report on additional archive observations from Gemini. These data were taken between 2004 and 2008 using the NIRI+Altair (adaptive optics instrument) and GNIRS instruments. These have resolving powers (λ/Δλ) of ~600 and 6000, respectively. Both data sets cover the K-band spectral range (1.95 to 2.40 μm) where gaseous CH4 has several strong lines, such as the ν3+ν4 Q-branch near 2.317 μm.Funding for this work has been provided by NASA-PATM grant NNX12AK62G.

Operation and performance of the New Horizons Long-Range Reconnaissance Imager during the Pluto encounter

NASA Astrophysics Data System (ADS)

Conard, S. J.; Weaver, H. A.; Núñez, J. I.; Taylor, H. W.; Hayes, J. R.; Cheng, A. F.; Rodgers, D. J.

2017-09-01

The Long-Range Reconnaissance Imager (LORRI) is a high-resolution imaging instrument on the New Horizons spacecraft. LORRI collected over 5000 images during the approach and fly-by of the Pluto system in 2015, including the highest resolution images of Pluto and Charon and the four much smaller satellites (Styx, Nix, Kerberos, and Hydra) near the time of closest approach on 14 July 2015. LORRI is a narrow field of view (0.29°), Ritchey-Chrétien telescope with a 20.8 cm diameter primary mirror and a three-lens field flattener. The telescope has an effective focal length of 262 cm. The focal plane unit consists of a 1024 × 1024 pixel charge-coupled device (CCD) detector operating in frame transfer mode. LORRI provides panchromatic imaging over a bandpass that extends approximately from 350 nm to 850 nm. The instrument operates in an extreme thermal environment, viewing space from within the warm spacecraft. For this reason, LORRI has a silicon carbide optical system with passive thermal control, designed to maintain focus without adjustment over a wide temperature range from -100 C to +50 C. LORRI operated flawlessly throughout the encounter period, providing both science and navigation imaging of the Pluto system. We describe the preparations for the Pluto system encounter, including pre-encounter rehearsals, calibrations, and navigation imaging. In addition, we describe LORRI operations during the encounter, and the resulting imaging performance. Finally, we also briefly describe the post-Pluto encounter imaging of other Kuiper belt objects and the plans for the upcoming encounter with KBO 2014 MU69.

The Search for Pluto Water

NASA Astrophysics Data System (ADS)

Cook, Jason C.; Cruikshank, Dale P.; Dalle Ore, Cristina M.; Ennico, Kimberly; Grundy, William M.; Olkin, Cathy B.; Protopapa, Silvia; Stern, S. Alan; Weaver, Harold A.; Young, Leslie A.

2015-11-01

On July 14, 2015, the New Horizons spacecraft made its closest approach to Pluto at about ~12,000 km from Pluto's surface. The LEISA (Linear Etalon Imaging Spectral Array) component of the Ralph instrument (Reuter, D.C., Stern, S.A., Scherrer, J., et al. 2008, Space Sci. Rev. 140, 129) obtained spatially resolved near infrared spectra at scales as small as 3 km/pix. LEISA covers the wavelength range 1.25 to 2.5 μm at a spectral resolution (λ/Δλ) of 240, and the 2.1 to 2.25 μm range at a resolution of 560. The observations from this instrument are being used to map the distribution of Pluto's known ices such as N2, CH4, CO and C2H6 as well as search for H2O-ice. To date, H2O-ice has evaded detection from Earth bound observatories. Observations based on LORRI, the LOng Range Reconnaissance Imager, suggest H2O-ice is a major component of several mountain ranges around the western perimeter of the landmass informally named Tombaugh Regio. If true, H2O-ice may be found in small isolated regions around Pluto. We will present our analysis of all LESIA data of Pluto in hand to search for and understand the distribution of H2O-ice. If found, we will also discuss limits on crystalline vs. amorphous H2O-ice and temperature measurements based on the 1.65 µm crystalline H2O-ice feature. This work was supported by NASA's New Horizons project.

Faces of Pluto Animation

NASA Image and Video Library

2015-06-11

This frame from a movie, composed of images taken by NASA New Horizons, shows Pluto as it rotates about its axis. The images were taken May 28-June 3, 2015, from distances ranging from approximately 56 million kilometers to 48.5 million kilometers.

Bladed Terrain on Pluto: Possible Origins and Evolution

NASA Technical Reports Server (NTRS)

Moore, J. M.; Howard, A. D.; Umurhan, O. M.; White, O. L.; Schenk, P. M.; Beyer, R. A.; Grundy, W. M.; Young, L. A.; Stern, S. A.; Weaver, H. A.;

The Phoenix Pluto Probe

NASA Technical Reports Server (NTRS)

Gunning, George R.; Spapperi, Jeff; Wilkinson, Jeffrey P.; Eldred, Jim; Labij, Dennis; Strinni, Meredith

1990-01-01

A design proposal for an unmanned probe to Pluto is presented. The topics covered include: (1) scientific instrumentation; (2) mission management, planning, and costing; (3) power and propulsion system; (4) structural subsystem; (5) command, control, and communication; and (6) attitude and articulation control.

The effect of sudden server breakdown on the performance of a disassembly line

NASA Astrophysics Data System (ADS)

Udomsawat, Gun; Gupta, Surendra M.

2005-11-01

Product and material recovery relies on the disassembly process to separate target components or materials from the end-of-life (EOL) products. Disassembly line is especially effective when products in large quantity are disassembled. Unlike an assembly line, a disassembly line is more complex and is subjected to numerous uncertainties including stochastic and multi-level arrivals of component demands, stochastic arrival times for EOL products, and process interruption due to equipment failure. These factors seriously impair the control mechanism in the disassembly line. A common production control mechanism is the traditional push system (TPS). TPS responds to the aforementioned complications by carrying substantial amounts of inventories. An alternative control mechanism is a newly developed multi-kanban pull system (MKS) that relies on dynamic routing of kanbans, which tends to minimize the system's inventories while maintaining demand serviceability. In this paper we explore the impact of sudden breakdown of server on the performance of a disassembly line. We compare the overall performances of the TPS and MKS by considering two scenarios. We present the solution procedure and results for these cases.

Comparative planetary nitrogen atmospheres: Density and thermal structures of Pluto and Triton

NASA Astrophysics Data System (ADS)

Strobel, Darrell F.; Zhu, Xun

2017-07-01

Both atmospheres of Pluto and Neptune's largest satellite Triton have cold surfaces with surface gravitational accelerations and atmospheric surface pressures of comparable magnitude. To study their atmospheres we have updated Zhu et al. (2014) model for Pluto's atmosphere by adopting Voigt line profiles in the radiation module with the latest spectral database and extended the model to Triton's atmosphere by including additional parameterized heating due to the magnetospheric electron transport and energy deposition. The CH4 mixing ratio profiles play central roles in differentiating the atmospheres of Pluto and Triton. On Pluto the surface CH4 mole fraction is in the range of 0.3-0.8%, sufficiently high to ensure that it is well mixed in the lower atmosphere and not subject to photochemical destruction. Near the exobase CH4 attains comparable density to N2 due to gravitational diffusive separation and escapes at 500 times the N2 rate (= 1 × 1023 N2 s-1). In Triton's atmosphere, the surface CH4 mole fraction is on the order of 0.015%, sufficiently low to ensure that it is photochemically destroyed irreversibly in the lower atmosphere and that N2 remains the major species, even at the exobase. With solar EUV power only, Triton's upper thermosphere is too cold and magnetospheric heating, approximately comparable to the solar EUV power, is needed to bring the N2 tangential column number density in the 500-800 km range up to values derived from the Voyager 2 UVS observations (Broadfoot et al., 1989). Due to their cold exobase temperatures relative to the gravitational potential energy wells that N2 resides in, atmospheric escape from Triton and Pluto is not dominated by N2 Jeans escape but by CH4 from Pluto and H, C, N and H2 from Triton. The atmospheric thermal structure near the exobase is sensitive to the atmospheric escape rate only when it is significantly greater than 2 × 1027 amu s-1, above which enhanced Jeans escape and larger radial velocity adiabatically cools the atmosphere to a lower temperature. Finally we suggest that Pluto's thermosphere is a cold ∼ 70 K due to ablation of H2O molecules from the influx of dust grains detected by New Horizons Student Dust Counter.

Adaptive Optics Imaging of Pluto-Charon and the Discovery of a Moon aroun d the Asteroid 45 Eugenia: The Potential of Adaptive Optics in Planetary Astrono my

NASA Astrophysics Data System (ADS)

Close, L. M.; Merline, W. J.; Tholen, D.; Owen, T.; Roddier, F.; Dumas, C.

1999-12-01

We outline two separate projects which highlight the power of adaptive optics (AO) to aid planetary research. The first project utilized AO to resolve the Pluto-Charon system by producing 0.15" FWHM images. We used the University of Hawaii AO system (Roddier et al. PASP 103, 131,1991) at CFHT to obtain deep (20 min) narrow band images in/out the molecular bands of water and methane ices. Our images confirm that the variation of Pluto's albedo is mainly governed by the presence of methane ice over its surface, resulting in a lower albedo at 2.26 um than at 2.02 um. Our observations confirm also that Charon is mostly covered with water-ice (Buie et al. NATURE 329, 522,1987). See Tholen et al. (ICARUS submitted) for more details on these AO results. In another application of AO, we discovered a moon around asteroid 45 Eugenia by use of the PUEO AO facility at CFHT (Rigaut et al. PASP 110, 152, 1998). With PUEO we preformed a search for asteroidal satellites among two dozen asteroids, achieving moderate Strehl ratios (35%) and FWHM of about 0.12" at H band. During this survey, we detected a faint close companion to 45 Eugenia. The satellite was 6.14 magnitudes (at 1.65 um) fainter and located at most 0.75" from Eugenia. Without the ability of AO (to sharpen the contrast and increase the resolution to 0.1"), the detection of this companion would have been impossible with ground based-telescopes. The companion was found to be in a 1200 km circular orbit with a period of 4.7 days. A more detailed discussion of this new satellite is given by Merline et al. in this volume. Adaptive optics is entering a powerful new age as all the major ground based large telescopes are developing facility AO systems. Planetary astronomy is particularly well posed to take advantage of the diffraction-limited, near-IR images (0.050" FWHM) that will become commonplace at all 8 m facilities in the near future (It is already occurring on the KECK and GEMINI-North telescopes). In particular, we review plans for the NAOS/CONICA AO facility instrument at the ESO 8m VLT that will have first light in late 2000. It is planned that NAOS/CONICA will obtain K-band Strehl ratios of 60% with reference objects (extended up to 3") of brightness V=13 (or brighter). The instrument will allow guiding on faint V=15 sources (with Strehls 20 well as tracking planetary targets that have a velocity different from the guide source. The ability to carry out remote service observing and an automatic data reduction pipeline will make the ESO VLT AO system ideal for monitoring temporal changes in planetary targets and carrying out targets of opportunity programs in general. These AO observations were made possible by support from the NSF, NASA, SwRI, and ESO.

Designing and verifying a disassembly line approach to cope with the upsurge of end-of-life vehicles in China.

PubMed

Zhang, Chunliang; Chen, Ming

2018-06-01

An upsurge of end-of-life vehicles (ELVs) is emerging in China, which means a potential monumental environmental crisis. The approach of disassembly line is expected to be an effective solution to such increasing volumes. Due to the complexity of vehicle product and uncertainties of disassembly processes, a complete set of disassembly line system should be taken into detailed consideration. We have designed and constructed a novel disassembly line using a flexible transition technique with the objective of complete disassembly. Prior to productivity testing, comparative Arena-based simulations on four scenarios have been performed and finally a best scenario is selected. The results show that the guarantee of cycle time is the key to meet the productivity target of 30,000 vehicles for one year. To achieve it, some constructive measures such as forcible entry tools are given. Copyright © 2018 Elsevier Ltd. All rights reserved.

Craters of All Ages and Sizes

NASA Image and Video Library

2015-11-10

Locations of more than 1,000 craters mapped on Pluto by NASA New Horizons mission indicate a wide range of surface ages, which likely means that Pluto has been geologically active throughout its history. http://photojournal.jpl.nasa.gov/catalog/PIA20154

The Rich Color Variations of Pluto

NASA Image and Video Library

2015-09-24

NASA's New Horizons spacecraft captured this high-resolution enhanced color view of Pluto on July 14, 2015. The image combines blue, red and infrared images taken by the Ralph/Multispectral Visual Imaging Camera (MVIC). Pluto's surface sports a remarkable range of subtle colors, enhanced in this view to a rainbow of pale blues, yellows, oranges, and deep reds. Many landforms have their own distinct colors, telling a complex geological and climatological story that scientists have only just begun to decode. The image resolves details and colors on scales as small as 0.8 miles (1.3 kilometers). http://photojournal.jpl.nasa.gov/catalog/PIA19952

The Pluto Affair: The good, the bad or the ugly?

NASA Astrophysics Data System (ADS)

Lindberg Christensen, Lars

2007-08-01

The International Astronomical Union (IAU) General Assembly in Prague 2006 was the setting of one of the most discussed stories of 2006 - the much hated and loved IAU Resolution to define a planet. The Resolution changed Pluto's status to a dwarf planet and resulted in an unprecedented emotional discussion. The author will start the discussion with some first-hand impressions of the events with the perspective of the IAU Press Officer. The discussion can then address other impressions of what happened in Prague. What were the negative and positive outcomes of the Pluto Affair? What can we learn from this experience?

NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy o

NASA Image and Video Library

2014-08-25

Dr. John Spencer, senior scientist at the Southwest Research Institute, left, Dr. Jeffrey Moore, senior scientist at NASA Ames Researh Center, center, and Dr. David H. Grinspoon, senior scientist at the Plentary Science Institute, left, are seen during a panel discussion at the "NASA's New Horizons Pluto Mission: Continuing Voyager's Legacy of Exploration" event on Monday, August, 25, 2014, in the James E. Webb Auditorium at NASA Headquarters in Washington, DC. The panelists gave their accounts of Voyager's encounter with Neptune and discussed their current assignments on NASA's New Horizons mission to Pluto. Photo Credit: (NASA/Joel Kowsky)

Magnitudes of selected stellar occultation candidates for Pluto and other planets, with new predictions for Mars and Jupiter

NASA Technical Reports Server (NTRS)

Sybert, C. B.; Bosh, A. S.; Sauter, L. M.; Elliot, J. L.; Wasserman, L. H.

1992-01-01

Occultation predictions for the planets Mars and Jupiter are presented along with BVRI magnitudes of 45 occultation candidates for Mars, Jupiter, Saturn, Uranus, and Pluto. Observers can use these magnitudes to plan observations of occultation events. The optical depth of the Jovian ring can be probed by a nearly central occultation on 1992 July 8. Mars occults an unusually red star in early 1993, and the occultations for Pluto involving the brightest candidates would possibly occur in the spring of 1992 and the fall of 1993.

Pluto in Extended Color

NASA Image and Video Library

2015-09-24

This cylindrical projection map of Pluto, in enhanced, extended color, is the most detailed color map of Pluto ever made by NASA New Horizons. It uses recently returned color imagery from the New Horizons Ralph camera, which is draped onto a base map of images from the NASA's spacecraft's Long Range Reconnaissance Imager (LORRI). The map can be zoomed in to reveal exquisite detail with high scientific value. Color variations have been enhanced to bring out subtle differences. Colors used in this map are the blue, red, and near-infrared filter channels of the Ralph instrument. http://photojournal.jpl.nasa.gov/catalog/PIA19956

Does Pluto Have a Haze Layer?

NASA Technical Reports Server (NTRS)

Elliot, James L.

1997-01-01

The goal of this research was to determine whether Pluto has a haze layer through observations (with the Kuiper Airborne Observatory) of a stellar occultation by Pluto that was originally predicted to occur on 1993 October 3. As described in the attached material, our extensive astrometric measurements determined that this occultation would not be visible from Earth, and we canceled plans to observe it with the KAO. Efforts were then directed toward improving our astrometric techniques so that we could find future occultations with which we could satisfy the original goals of the research proposed for this grant.

Detection of Gaseous Methane on Pluto

NASA Technical Reports Server (NTRS)

Young, Leslie; Tokunaga, Alan; Elliot, J.; deBergh, Catherine; Owen, Tobias; Witteborn, Fred C. (Technical Monitor)

1995-01-01

We obtained Pluto's spectrum using the CSHELL echelle spectrograph at NASA's IRTF on Mauna Kea, on 25-26 May 1992, with a spectral resolution of 13,300. The spectral range (5998 - 6018 per centimeter, or 1661.8 - 1666.9 nm) includes the R(0) and the Q(1) - Q(9) lines of the 2v3 band of methane. The resulting spectrum shows the first detection of gaseous methane on Pluto, with a column height of 1.20 (sup +3.15) (sub -0.87) cm-A (3.22 (sup +8.46) (sub -2.34) x 10(exp 19) molecule per square centimeter)).

Beyond Pluto: The Search for the Edge of the Solar System

DOE Office of Scientific and Technical Information (OSTI.GOV)

Funsten, Herb

In July, we finally visited the last major body of our solar system, Pluto. But what lies beyond? The stellar wind from our Sun forms an enormous bubble in interstellar space. This “sphere of our Sun,” or heliosphere, extends far beyond Pluto and forms a protective cocoon that shields us from cosmic radiation. In this talk, we will travel to the edge of the solar system, peer into the structure and dynamics of the outer heliosphere as it interacts with the interstellar medium and anticipate the future of the solar system as it moves through our galactic neighborhood.

Project Cerberus: Flyby Mission to Pluto

NASA Technical Reports Server (NTRS)

Sivier, K.; Koepke, A.; Humphrey, Theodore W.; Elbel, Jeffrey P.; Hackett, Bruce E.; Kennedy, Ralph G.; Leo, Donald J.; Zimmerman, Shery A.

1990-01-01

The goal of the Cerberus Project was to design a feasible and cost-effective unmanned flyby mission to Pluto. The requirements in the request for proposal for an unmanned probe to Pluto are presented and were met. The design stresses proven technology that will avoid show stoppers which could halt mission progress. Cerberus also utilizes the latest advances in the spacecraft industry to meet the stringent demands of the mission. The topics covered include: (1) mission management, planning, and costing; (2) structures; (3) power and propulsion; (4) attitude, articulation, and control; (5) command, control, and communication; and (6) scientific instrumentation.

Comparative mapping of Pluto's sub-Charon hemisphere - Three least squares models based on mutual event lightcurves

NASA Technical Reports Server (NTRS)

Young, Eliot F.; Binzel, Richard P.

1993-01-01

Observations of Charon transits are used here to derive preliminary maps of Pluto's sub-Charon hemisphere. Three models are used to describe the brightness of Pluto's surface as functions of latitude and longitude. Mapping results are presented using spherical harmonic functions, polynomial functions, and finite elements. A smoothing algorithm applied to the maps is described and the validity and resolution of the maps is tested by reconstruction from synthetic data. A preliminary finding from the maps is that the south polar region has the highest albedo of any location on the planet.

The Global Color of Pluto from New Horizons

NASA Astrophysics Data System (ADS)

Olkin, Catherine B.; Spencer, John R.; Grundy, William M.; Parker, Alex H.; Beyer, Ross A.; Schenk, Paul M.; Howett, Carly J. A.; Stern, S. Alan; Reuter, Dennis C.; Weaver, Harold A.; Young, Leslie A.; Ennico, Kimberly; Binzel, Richard P.; Buie, Marc W.; Cook, Jason C.; Cruikshank, Dale P.; Dalle Ore, Cristina M.; Earle, Alissa M.; Jennings, Donald E.; Singer, Kelsi N.; Linscott, Ivan E.; Lunsford, Allen W.; Protopapa, Silvia; Schmitt, Bernard; Weigle, Eddie; the New Horizons Science Team

2017-12-01

The New Horizons flyby provided the first high-resolution color maps of Pluto. We present here, for the first time, an analysis of the color of the entire sunlit surface of Pluto and the first quantitative analysis of color and elevation on the encounter hemisphere. These maps show the color variation across the surface from the very red terrain in the equatorial region, to the more neutral colors of the volatile ices in Sputnik Planitia, the blue terrain of East Tombaugh Regio, and the yellow hue on Pluto’s North Pole. There are two distinct color mixing lines in the color-color diagrams derived from images of Pluto. Both mixing lines have an apparent starting point in common: the relatively neutral-color volatile-ice covered terrain. One line extends to the dark red terrain exemplified by Cthulhu Regio and the other extends to the yellow hue in the northern latitudes. There is a latitudinal dependence of the predominant color mixing line with the most red terrain located near the equator, less red distributed at mid-latitudes and more neutral terrain at the North Pole. This is consistent with the seasonal cycle controlling the distribution of colors on Pluto. Additionally, the red color is consistent with tholins. The yellow terrain (in the false color images) located at the northern latitudes occurs at higher elevations.

Pluto and Charon's Visible Spectrum (3500-9000 Å)

NASA Astrophysics Data System (ADS)

Cook, J. C.; Wyckoff, S.

2003-05-01

Uncertainty in the chemical composition of Pluto's atmosphere severely limits our understanding of its physical properties. The only atmospheric gas identified spectroscopically to date has been CH4 (Young et al., 1997), while an upper limit has been set for CO gas (Young et al., 2001). Infrared detection of surface N2 ice (Owen et al., 1993) together with models based on occultation data (Elliot and Young, 1992) indicate that Pluto's atmosphere is probably dominated by CO and/or N2 (Yelle and Lunine, 1989; Hubbard et al., 1990; Stansberry et al., 1994). If the atmosphere is in vapor pressure equilibrium with the surface ice, then N2 gas would dominate the atmosphere with abundances ≳ 90% (Owen et al., 1993). Here we report on a search to identify atmospheric spectral features using data collected with the Steward Observatory 90'' Bok Telescope and the B & C Spectrograph. Pluto-Charon spectra were obtained on five nights in May and June 2003 using 300 l/mm grating blazed in the blue and red spectral regions. We present spectra covering the visible range from 3500 to 9000 Å : (λ /Δ λ ˜ 750 at 6000 Å), and discuss limits set on gases in the atmosphere and extended exosphere of the Pluto-Charon system. J. C. Cook would like to acknowledge support from NASA Space Grant Fellowship.

Ices on Charon: Distribution of H2O and NH3 from New Horizons LEISA observations

NASA Astrophysics Data System (ADS)

Dalle Ore, C. Morea; Protopapa, S.; Cook, J. C.; Grundy, W. M.; Cruikshank, D. P.; Verbiscer, A. J.; Ennico, K.; Olkin, C. B.; Stern, S. A.; Weaver, H. A.; Young, L. A.; New Horizons Science Team

2018-01-01

Charon, the largest moon of Pluto, appeared as a fairly homogeneous, gray, icy world to New Horizons during closest approach on July 14th, 2015. Charon's sub-Pluto hemisphere was scanned by the Ralph/LEISA near-IR spectrograph providing an unprecedented opportunity to measure its surface composition. We apply a statistical clustering tool to identify spectrally distinct terrains and a radiative transfer approach to study the variations of the 2.0-μm H2O ice band. We map the distribution of the ices previously reported to be present on Charon's surface, namely H2O and the products of NH3 in H2O. We find that H2O ice is mostly in the crystalline phase, confirming previous studies. The regions with the darkest albedos show the strongest signature of amorphous-phase ice, although the crystalline component is still strong. The brighter albedo regions, often corresponding to crater ejecta blankets, are characterized by larger H2O grains, possibly an indication of a younger age. We observe two different behaviors for the two absorption bands representing NH3 in H2O. The 2.21-μm band tends to cluster more in the northern areas compared to the ∼2.01-μm band. Both bands are present in the brighter crater rays, but not all craters show both bands. The 2.21-μm band is also clearly present on the smaller moons Hydra and Nix. These results hint that different physical conditions may determine the appearance or absence of these two different forms of NH3 in H2O ice in the Pluto system. We also investigate the blue slope affecting the spectrum at wavelengths longer than ∼1.8 μm previously reported by several authors. We find that the slope is common among the objects in the Pluto system, Charon, the smaller moons Nix and Hydra, and the darkest terrains on Pluto. It also characterizes the analog ice tholin obtained from irradiation of Pluto-specific materials (a mixture of N2, CH4, and CO ices) in the laboratory. Our modeling results show that Pluto ice tholins are widespread almost uniformly on Charon suggesting a common distribution possibly part of the original reservoir of materials that made up Charon. This was irradiated over the years to yield the gray color characteristic of Charon today. On top of the 'primordial' Pluto ice tholin there is the redder component produced by irradiation of the CH4 provided by Pluto's atmospheric contribution as illustrated by Grundy et al. (2016a).

Cost-assessment Analysis of Local Vehicle Scrapping Facility

NASA Astrophysics Data System (ADS)

Grabowski, Lukasz; Gliniak, Maciej; Polek, Daria; Gruca, Maria

2017-12-01

The purpose of the paper was to analyse the costs of recycling vehicles at local vehicle scrapping facility. The article contains regulations concerning vehicle decommissioning, describes the types of recovery, vehicles recycling networks, analyses the structure of a disassembly station, as well as the financial and institutional system in charge of dealing with the recycling of vehicles in Poland. The authors present the number of scrapped vehicles at local recycling company and the level of achieved recovery and recycling. The research presented in the article shows financial situation of the vehicle scrapping industry. In addition, it has been observed that the number of subsidies are directly proportional to the number of scrapped vehicles, and achieved levels of recycling and recovery depends on the percentage of incomplete vehicles.

Guide of good practices for occupational radiological protection in plutonium facilities

DOE Office of Scientific and Technical Information (OSTI.GOV)

NONE

1998-06-01

This Technical Standard (TS) does not contain any new requirements. Its purpose is to provide guides to good practice, update existing reference material, and discuss practical lessons learned relevant to the safe handling of plutonium. the technical rationale is given to allow US Department of Energy (DOE) health physicists to adapt the recommendations to similar situations throughout the DOE complex. Generally, DOE contractor health physicists will be responsible to implement radiation protection activities at DOE facilities and DOE health physicists will be responsible for oversight of those activities. This guidance is meant to be useful for both efforts. This TSmore » replaces PNL-6534, Health Physics Manual of Good Practices for Plutonium Facilities, by providing more complete and current information and by emphasizing the situations that are typical of DOE`s current plutonium operations; safe storage, decontamination, and decommissioning (environmental restoration); and weapons disassembly.« less

Application of industrial robots in automatic disassembly line of waste LCD displays

NASA Astrophysics Data System (ADS)

Wang, Sujuan

2017-11-01

In the automatic disassembly line of waste LCD displays, LCD displays are disassembled into plastic shells, metal shields, circuit boards, and LCD panels. Two industrial robots are used to cut metal shields and remove circuit boards in this automatic disassembly line. The functions of these two industrial robots, and the solutions to the critical issues of model selection, the interfaces with PLCs and the workflows were described in detail in this paper.

KSC-05pd2542

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - Inside NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, workers push the newly arrived third stage, or upper stage for the New Horizons spacecraft, into position for uncovering. The third stage is a Boeing STAR 48 solid-propellant kick motor. The Atlas V is the launch vehicle for NASA’s New Horizons spacecraft, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11 and fly through the Pluto system as early as summer 2015. New Horizons will be powered by a single radioisotope thermoelectric generator (RTG), provided by the Department of Energy, which will be installed shortly before launch.

KSC-05pd2539

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - Before dawn, the third stage, or upper stage for the New Horizons spacecraft, arrives at NASA Kennedy Space Center’s Payload Hazardous Servicing Facility. The third stage is a Boeing STAR 48 solid-propellant kick motor. The Atlas V is the launch vehicle for NASA’s New Horizons spacecraft, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11 and fly through the Pluto system as early as summer 2015. New Horizons will be powered by a single radioisotope thermoelectric generator (RTG), provided by the Department of Energy, which will be installed shortly before launch.

KSC-05pd2541

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - The third stage, or upper stage for the New Horizons spacecraft, is moved toward the open door of NASA Kennedy Space Center’s Payload Hazardous Servicing Facility. The third stage is a Boeing STAR 48 solid-propellant kick motor. The Atlas V is the launch vehicle for NASA’s New Horizons spacecraft, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11 and fly through the Pluto system as early as summer 2015. New Horizons will be powered by a single radioisotope thermoelectric generator (RTG), provided by the Department of Energy, which will be installed shortly before launch.

KSC-05pd2540

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - The third stage, or upper stage for the New Horizons spacecraft, is moved toward the open door of NASA Kennedy Space Center’s Payload Hazardous Servicing Facility. The third stage is a Boeing STAR 48 solid-propellant kick motor. The Atlas V is the launch vehicle for NASA’s New Horizons spacecraft, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11 and fly through the Pluto system as early as summer 2015. New Horizons will be powered by a single radioisotope thermoelectric generator (RTG), provided by the Department of Energy, which will be installed shortly before launch.

KSC-05pd2543

NASA Image and Video Library

2005-12-01

KENNEDY SPACE CENTER, FLA. - Inside NASA Kennedy Space Center’s Payload Hazardous Servicing Facility, workers remove the protective cover from around the newly arrived third stage, or upper stage for the New Horizons spacecraft. The third stage is a Boeing STAR 48 solid-propellant kick motor. The Atlas V is the launch vehicle for NASA’s New Horizons spacecraft, scheduled to launch from Cape Canaveral Air Force Station, Fla., during a 35-day window that opens Jan. 11 and fly through the Pluto system as early as summer 2015. New Horizons will be powered by a single radioisotope thermoelectric generator (RTG), provided by the Department of Energy, which will be installed shortly before launch.

Compaction-Driven Evolution of Pluto's Rocky Core: Implications for Water-Rock Interactions

NASA Astrophysics Data System (ADS)

Gabasova, L. R.; Tobie, G.; Choblet, G.

2018-05-01

We model the compaction of Pluto's rocky core after accretion and explore the potential for hydrothermal circulation within the porous layer, as well as examine its effect on core cooling and the persistence of a liquid internal ocean.

The Prolyl Isomerase Pin1 Promotes the Herpesvirus-Induced Phosphorylation-Dependent Disassembly of the Nuclear Lamina Required for Nucleocytoplasmic Egress.

PubMed

Milbradt, Jens; Hutterer, Corina; Bahsi, Hanife; Wagner, Sabrina; Sonntag, Eric; Horn, Anselm H C; Kaufer, Benedikt B; Mori, Yasuko; Sticht, Heinrich; Fossen, Torgils; Marschall, Manfred

2016-08-01

The nuclear lamina lines the inner nuclear membrane providing a structural framework for the nucleus. Cellular processes, such as nuclear envelope breakdown during mitosis or nuclear export of large ribonucleoprotein complexes, are functionally linked to the disassembly of the nuclear lamina. In general, lamina disassembly is mediated by phosphorylation, but the precise molecular mechanism is still not completely understood. Recently, we suggested a novel mechanism for lamina disassembly during the nuclear egress of herpesviral capsids which involves the cellular isomerase Pin1. In this study, we focused on mechanistic details of herpesviral nuclear replication to demonstrate the general importance of Pin1 for lamina disassembly. In particular, Ser22-specific lamin phosphorylation consistently generates a Pin1-binding motif in cells infected with human and animal alpha-, beta-, and gammaherpesviruses. Using nuclear magnetic resonance spectroscopy, we showed that binding of Pin1 to a synthetic lamin peptide induces its cis/trans isomerization in vitro. A detailed bioinformatic evaluation strongly suggests that this structural conversion induces large-scale secondary structural changes in the lamin N-terminus. Thus, we concluded that a Pin1-induced conformational change of lamins may represent the molecular trigger responsible for lamina disassembly. Consistent with this concept, pharmacological inhibition of Pin1 activity blocked lamina disassembly in herpesvirus-infected fibroblasts and consequently impaired virus replication. In addition, a phospho-mimetic Ser22Glu lamin mutant was still able to form a regular lamina structure and overexpression of a Ser22-phosphorylating kinase did not induce lamina disassembly in Pin1 knockout cells. Intriguingly, this was observed in absence of herpesvirus infection proposing a broader importance of Pin1 for lamina constitution. Thus, our results suggest a functional model of similar events leading to disassembly of the nuclear lamina in response to herpesviral or inherent cellular stimuli. In essence, Pin1 represents a regulatory effector of lamina disassembly that promotes the nuclear pore-independent egress of herpesviral capsids.

The Prolyl Isomerase Pin1 Promotes the Herpesvirus-Induced Phosphorylation-Dependent Disassembly of the Nuclear Lamina Required for Nucleocytoplasmic Egress

PubMed Central

Milbradt, Jens; Hutterer, Corina; Bahsi, Hanife; Wagner, Sabrina; Sonntag, Eric; Kaufer, Benedikt B.; Mori, Yasuko; Sticht, Heinrich; Fossen, Torgils; Marschall, Manfred

2016-01-01

The nuclear lamina lines the inner nuclear membrane providing a structural framework for the nucleus. Cellular processes, such as nuclear envelope breakdown during mitosis or nuclear export of large ribonucleoprotein complexes, are functionally linked to the disassembly of the nuclear lamina. In general, lamina disassembly is mediated by phosphorylation, but the precise molecular mechanism is still not completely understood. Recently, we suggested a novel mechanism for lamina disassembly during the nuclear egress of herpesviral capsids which involves the cellular isomerase Pin1. In this study, we focused on mechanistic details of herpesviral nuclear replication to demonstrate the general importance of Pin1 for lamina disassembly. In particular, Ser22-specific lamin phosphorylation consistently generates a Pin1-binding motif in cells infected with human and animal alpha-, beta-, and gammaherpesviruses. Using nuclear magnetic resonance spectroscopy, we showed that binding of Pin1 to a synthetic lamin peptide induces its cis/trans isomerization in vitro. A detailed bioinformatic evaluation strongly suggests that this structural conversion induces large-scale secondary structural changes in the lamin N-terminus. Thus, we concluded that a Pin1-induced conformational change of lamins may represent the molecular trigger responsible for lamina disassembly. Consistent with this concept, pharmacological inhibition of Pin1 activity blocked lamina disassembly in herpesvirus-infected fibroblasts and consequently impaired virus replication. In addition, a phospho-mimetic Ser22Glu lamin mutant was still able to form a regular lamina structure and overexpression of a Ser22-phosphorylating kinase did not induce lamina disassembly in Pin1 knockout cells. Intriguingly, this was observed in absence of herpesvirus infection proposing a broader importance of Pin1 for lamina constitution. Thus, our results suggest a functional model of similar events leading to disassembly of the nuclear lamina in response to herpesviral or inherent cellular stimuli. In essence, Pin1 represents a regulatory effector of lamina disassembly that promotes the nuclear pore-independent egress of herpesviral capsids. PMID:27556400

ASICs for the Pluto Energetic Particle Spectrometer Science Investigation on NASA's New Horizons mission to Pluto

NASA Astrophysics Data System (ADS)

Paschalidis, Nicholas; McNutt, Ralph

One of the most critical challenges of the Pluto Energetic Particle Spectrometer Science Inves-tigation (PEPSSI) was to meet the science requirements with a total mass and power of ¡1.5 kg and ¡2.5 W, respectively. A key, enabling technology to achieve these goals was the exten-sive use of high-performance, low-power, application-specific integrated circuits (ASICs) for the miniaturization of the 12-channel solid state detector (SSD) readout system, the time-of-flight (TOF) system, and the power supply and housekeeping systems. The PEPSSI instrument is a TOF-versus-energy, compact particle spectrometer that provides measurements of ions and electrons from 20keV to 1MeV in a 160 x 12 solid angle field of view divided into six dual-channel sectors. TOF, constant fraction discriminator (CFD), energy, peak detector, and temperature, remote input/output (TRIO, housekeeping) ASICs were all used synergistically in the instrument enabling the high science performance within the resource constraints. The ASICs were space qualified in accord with military specifications (Class S) for total radiation dose and single-event effects (SEEs), and, most importantly, for a 2000-hour life test to increase the reliability for the long duration of the mission. PEPSSI flies on-board the New Horizons NASA spacecraft to measure pick-up ions from the Pluto's outgassing atmosphere. The space-craft was launched 19 Jan 2006 and presently is en route to Pluto, having passed Jupiter in early 2007. Closest approach to Pluto will occur in mid-July 2015. The instrument has already produced excellent measurements in interplanetary space and during the traversal of Jupiter's magnetotail in 2007.

Pluto Icy Plains Captured in Highest-Resolution Views from New Horizons

NASA Image and Video Library

2016-01-08

NASA's New Horizons spacecraft continues to transmit the sharpest views of Pluto that it obtained (and recorded) during its flyby of the distant planet on July 14, 2015. The newest image, returned on Dec. 24, 2015, extends New Horizons' highest-resolution swath of Pluto to the very center of the informally named Sputnik Planum, and nearly completes the set of highest-resolution images taken by New Horizons last July. The pictures are part of a sequence taken near New Horizons' closest approach to Pluto, with resolutions of about 250-280 feet (77-85 meters) per pixel -- revealing features smaller than half a city block on Pluto's surface. The images shown here form a strip 50 miles (80 kilometers) wide and more than 400 miles (700 kilometers) long, trending from the northwestern shoreline of Sputnik Planum and out across its icy plains. The images illustrate the polygonal or cellular pattern of the plains, which are thought to result from the convective churning of a deep layer solid, but mobile, nitrogen ice. The surface of Sputnik Planum appears darker toward the shore (at top), possibly implying a change in composition or surface texture. The occasional raised, darker blocks at the cell edges are probably dirty water "icebergs" floating in denser solid nitrogen. The pictures were taken with the telescopic Long Range Reconnaissance Imager (LORRI) aboard New Horizons, from a range of approximately 10,000 miles (17,000 kilometers) over a timespan of about a minute centered on 11:36 UT on July 14 -- just about 15 minutes before New Horizons' closest approach to Pluto. http://photojournal.jpl.nasa.gov/catalog/PIA20336

Photochemistry of Pluto's Atmosphere

NASA Technical Reports Server (NTRS)

Krasnopolsky, Vladimir A.

1999-01-01

This work include studies of two problems: (1) Modeling thermal balance, structure. and escape processes in Pluto's upper atmosphere. This study has been completed in full. A new method, of analytic solution for the equation of hydrodynamic flow from in atmosphere been developed. It was found that the ultraviolet absorption by methane which was previously ignored is even more important in Pluto's thermal balance than the extreme ultraviolet absorption by nitrogen. Two basic models of the lower atmosphere have been suggested, with a tropopause and a planetary surface at the bottom of the stellar occultation lightcurve, respectively, Vertical profiles, of temperature, density, gas velocity, and the CH4 mixing ratio have been calculated for these two models at low, mean, and high solar activity (six models). We prove that Pluto' " s atmosphere is restricted to 3060-4500 km, which makes possible a close flyby of future spacecraft. Implication for Pluto's evolution have also been discussed. and (2) Modeling of Pluto's photochemistry. Based on the results of (1), we have made some changes in the basic continuity equation and in the boundary conditions which reflect a unique can of hydrodynamic escape and therefore have not been used in modeling of other planetary atmospheres. We model photochemistry of 44 neutral and 23 ion species. This work required solution of a set of 67 second-order nonlinear ordinary differential equations. Two models have been developed. Each model consists of the vertical profiles for 67 species, their escape and precipitation rates. These models predict the chemical structure and basic chemical processes in the current atmosphere and possible implication of these processes for evolution. This study has also been completed in full.

Pluto Fast Flyby: An Overview of the Mission and Spacecraft Design, Advanced Technology Insertion Efforts, and Student Involvement Opportunities

NASA Technical Reports Server (NTRS)

Abraham, D. S.; Staehle, R.; Brewster, S.; Caldwell, D.; Carraway, J.; Henry, P.; Herman, M.; Kissel, G.; Peak, S.; Randolph, V.;

The Prolonged Downfall of the Democratic Republic of Afghanistan

DTIC Science & Technology

2014-05-22

Afghanistan (London, UK: Pluto Press, 2001); Gilles Dorronsoro, Revolution Unending: Afghanistan, 1979 to the Present, trans. John King (New York, NY...2 (May 2007): 235-61. Griffin, Michael. Reaping the Whirlwind: The Taliban Movement in Afghanistan. London, UK: Pluto Press, 2001. Jalali, Ali

The Campaign for the Occultation of UCAC4-347-165728 (R=12m2) by Pluto on June 29th, 2015

NASA Astrophysics Data System (ADS)

Beisker, W.; Sicardy, B.; Berard, D.; Meza, E.; Herald, D.; Gault, D.; Talbot, J.; Bode, H.-J.; Braga-Ribas, F.; Barry, T.; Broughton, J.; Hanna, W.; Bradshaw, J.; Kerr, S.; Pavlov, H.

2015-10-01

The occultation of UCAC4-347-165728 (R=12m2)on the 29th of June 2015 by Pluto is the last important occultation by Pluto before the New Horizons flyby 15 days later. Therefore it is a great opportunity to measure details of Pluto's atmosphere from Earth at the same time as the "on-site" determination. Observations from mobile stations and from certain fixed site observatories are planned in an international campaign in Australia and New Zealand. The telescopes will be equipped with EMCCD or CCD cameras to record a frame sequence linked to the exact timing by GPS. With high resolution astrometry in the months and weeks before the event, we intend to define the central line of the occultation so accurate that a positioning of instruments in close proximity of the central line is possible. - First results of the campaign will be presented in this report.