Sample records for aarma jaan vainu

  1. Occultation of 2UCAC 42376428 by (423) Diotima on 2005 March 06

    NASA Astrophysics Data System (ADS)

    Vasundhara, R.; Kuppuswamy, K.; Ramamoorthy, S.; Velu, C.; Venkataramana, A. K.

    2006-03-01

    Observations of the occultation of the star 2UCAC 42376428 by (423) Diotima on 2005 March 06 at the Vainu Bappu Observatory are reported. The observed mid time of the event at 15:12:25.1 UT occurred 3.4 s later than the predicted time but within the 1 uncertainty of 4.3 s of the predictions by IOTA. The duration of the event of 4.2 s was found to be shorter than the predictions even allowing for a one sigma uncertainty in the impact parameter. This implies a narrower projected width of the asteroid along the occultation track at the time of the event.

  2. VizieR Online Data Catalog: BVR photometry of EPIC 211957146 (Sriram+, 2017)

    NASA Astrophysics Data System (ADS)

    Sriram, K.; Malu, S.; Choi, C. S.; Vivekananda Rao, P.

    2017-08-01

    Photometric observations of the variable EPIC 211957146 in the R band were taken using the IUCAA-Girawali Observatory (IGO) 2m telescope from 2015 February 5-22, for 5 nights (specifications of IGO 2m telescope CCD are as discussed in Sriram et al. 2016AJ....151...69S). An exposure time of 20-30s was given for imaging. B and V band observations were taken from the JCBT 1.3m telescope at Vainu Bappu Observatory (VBO) during 2016 February 3-8 and 2016 March 25-April 3 for a total of 7 nights. The JCBT 1.3m DFM telescope at VBO uses a 2K*4K UKATC CCD having a gain of 0.745e-/ADU and a read out noise of 4.2e-. The plate scale is 0.3arcsec/pixel resulting in an image of 10'*20' and images of the source in the B and V bands were taken with an integration time of 120s. Differential photometry was performed on the variable, with the comparison and check stars (of similar brightness) lying close to the variable. This source was also observed by the Kepler K2 mission Campaign 5, and the data were acquired from the MAST portal and the NASA Exoplanet Archive. K2 campaign 5 monitored the sky for a duration of ~74days and was fixed upon a single boresight position of 08h40m38s, +16°49'47'' starting from 2015 April 27 to July 10. Spectroscopic observation of the variable was performed during the nights of 2016 January 29-30 using the 2m Himalaya Chandra Telescope (HCT, IAO) equipped with the Himalaya Faint Object Spectrograph Camera (HFOSC) having a 2K*4K CCD. Spectra were obtained with an exposure time of 1800-2700s for both variable and spectrophotometric standard stars (BD+08 2015). A few spectra were also taken on 2016 February 1 using the Optomechanics Research spectrograph mounted on the 2.3m Vainu Bappu Telescope using a 1K*1K CCD. A 600lines/mm grating spanning a wavelength range of 2000-8000Å with a dispersion of 2.6Å/pixel and a resolution of ~5.3Å was used. The same spectrophotometric standard as before was used for observation, and an exposure time of 2700s was

  3. Social Contributions to the Equilibration of Action Schemes: A Longitudinal Study of Locomotion.

    ERIC Educational Resources Information Center

    Lightfoot, Cynthia

    According to Jaan Valsiner, development takes place within culturally structured environments jointly organized by the activities of children and the people around them. When overlap between promoted activity and the child's zone of proximal development exists, the structure of action that results from the interplay of the two is internalized by…

  4. US National Economic Security in a Global Market

    DTIC Science & Technology

    1990-01-01

    13 (D) the Secretary of Commerce , 14 ( E ) the Secretary of Treasury, 15 (F) the United States Trade Representative, 16 and _ 17 (G) the Director of...OTe F!LE COPY --- National Security Program 00 N US NATIONAL ECONOMIC SECURITY IN A GLOBAL MARKET :I . DTIC ELECTE JAN14 1991 m S E D HARVARD...importantly, will become 5 I I ,,!"C is merica _ _ _ _ 44% 5AlAN leact rustwrthv __ 29% ’,’EST (E7,1RM.’y ,a ]i,- :. . 8 %FFR ANC E - 5% BRITAIN Does Jaan

  5. Asteroseismology of RXJ 2117+3412, the hottest pulsating PG 1159 star

    NASA Astrophysics Data System (ADS)

    Vauclair, G.; Moskalik, P.; Pfeiffer, B.; Chevreton, M.; Dolez, N.; Serre, B.; Kleinman, S. J.; Barstow, M.; Sansom, A. E.; Solheim, J.-E.; Belmonte, J. A.; Kawaler, S. D.; Kepler, S. O.; Kanaan, A.; Giovannini, O.; Winget, D. E.; Watson, T. K.; Nather, R. E.; Clemens, J. C.; Provencal, J.; Dixson, J. S.; Yanagida, K.; Nitta Kleinman, A.; Montgomery, M.; Klumpe, E. W.; Bruvold, A.; O'Brien, M. S.; Hansen, C. J.; Grauer, A. D.; Bradley, P. A.; Wood, M. A.; Achilleos, N.; Jiang, S. Y.; Fu, J. N.; Marar, T. M. K.; Ashoka, B. N.; Meĭstas, E. G.; Chernyshev, A. V.; Mazeh, T.; Leibowitz, E.; Hemar, S.; Krzesiński, J.; Pajdosz, G.; Zoła, S.

    2002-01-01

    The pulsating PG 1159 planetary nebula central star RXJ 2117+3412 has been observed over three successive seasons of a multisite photometric campaign. The asteroseismological analysis of the data, based on the 37 identified l=1 modes among the 48 independent pulsation frequencies detected in the power spectrum, leads to the derivation of the rotational splitting, the period spacing and the mode trapping cycle and amplitude, from which a number of fundamental parameters can be deduced. The average rotation period is 1.16±0.05 days. The trend for the rotational splitting to decrease with increasing periods is incompatible with a solid body rotation. The total mass is 0.56+0.02-0.04 Msolar and the He-rich envelope mass fraction is in the range 0.013-0.078 M*. The luminosity derived from asteroseismology is log(L/Lsolar)= 4.05 +0.23-0.32 and the distance 760 +230-235 pc. At such a distance, the linear size of the planetary nebulae is 2.9±0.9 pc. The role of mass loss on the excitation mechanism and its consequence on the amplitude variations is discussed. Based on data obtained in observing time allocated by the Bernard Lyot Telescope, INSU/CNRS, France, the TCS at Teide Observatory, Tenerife, Spain, the INT and JKT Telescopes at Roque de Los Muchachos Observatory, La Palma, Spain, the Laboratorio Nacional de Astrofisica/CNPq, Brazil, the McDonal Observatory, Texas, USA, the Steward Observatory, Arizona, USA, the Mauna Kea Observatory, University of Hawaii, USA, the Mount Stromlo and Siding Spring Observatory, Australia, the Beijing Observatory, China, the Vainu Bappu Observatory, India, the Maidanak Observatory, Uzbekistan, the Wise Observatory, Israel, and the Suhora Observatory, Poland.

  6. An Introduction to Human Resource Development in Taiwan, R.O.C. = Jong Hwa Min Gwo Ren Li Tz Yuan Fa Jaan Jyan Jieh.

    ERIC Educational Resources Information Center

    Lee, Lung-Sheng; Chen, Ya-Yan

    In Taiwan, human resource development (HRD) is defined as the systematic education, training, and development employers provide for their employees as well as organizational development for corporations. A history of HRD development indicates that in the 1960s, the government began to implement planning measures for HRD in business and industry;…

  7. Vygotsky's Fragile Genius in Time and Place: Essay Review of "Understanding Vygotsky: A Quest for Synthesis" by Rene van der Veer and Jaan Valsiner.

    ERIC Educational Resources Information Center

    Youniss, James

    1994-01-01

    Briefly summarizes Vygotsky's life, the appeal and subsequent abandonment of his ideas in the 1960s, and renewal of interest in the 1970s and 1980s (often at the expense of Piaget). Praises van der Veer and Valsinger's book as a realistic picture of Vygotsky's background, life, and work, of the scientific and political context in Russia and of his…

  8. Stakeholder analysis of perceived relevance of connectivity - the implication to your research

    NASA Astrophysics Data System (ADS)

    Smetanova, Anna; Müller, Eva Nora Nora; Fernández-Getino, Ana Patricia; José Marqués, María; Vericat, Damià; Dugodan, Recep; Kapovic, Marijana; Ljusa, Melisa; Ferreira, Carla Sofia; Cavalli, Marco; Marttila, Hannu; Broja, Manuel Esteban Lucas; Święchowicz, Jolanta; Zumr, David

    2016-04-01

    conducting interview with a stakeholder: Charles Bielders (Catholic University Louvain, Belgium), Frédéric Darboux (Department of Soil Science Orléans, INRA, France), Dragana Dordevic (Centre of Chemistry, University of Belgrade, Serbia), Tobias Heckmann (Catholic University of Eichstätt-Ingolstadt, Germany), Anna Kidová (Institute of Geography, Slovak Academy of Sciences, Slovakia), Tobias Krüger (Integrative Research Institute on Transformations of Human-Environment Systems, Humboldt University, Germany), Carly Maynard (Department of Geography and the Lived Environment, University of Edinburgh, UK), Eva Mockler, (School of Civil, Structural and Environmental Engineering , University College Dublin, Ireland), Tony Parsons, (Department of Geography, University Sheffield, UK), Thorunn Petursdottir (RECARE, Soil Conservation Service of Iceland, Iceland), Ronald Pöppel (Institute of Geography and Regional Research, University Vienna, Austria), Jerzy Rejman (Institute of Agronomy, Polish Academy of Sciences, Poland), Jose López-Tarazón (Institute of Earth and Environmental Sciences, University of Potsdam, Germany), Sophie Tindale (Department of Geography, University, Durham, UK), Brigitta Tóth (Department of Crop Production and Soil Sciences, Pannonian University, Hungary) and Marco Vainu (Institute of Ecology, Tallinn University, Estonia). The project was supported by COST-STSM-ECOST-STSM-ES1306-011215-063624.

  9. Analysis of the Type IV Fimbrial-Subunit Gene fimA of Xanthomonas hyacinthi: Application in PCR-Mediated Detection of Yellow Disease in Hyacinths

    PubMed Central

    van Doorn, J.; Hollinger, T. C.; Oudega, B.

    2001-01-01

    A sensitive and specific detection method was developed for Xanthomonas hyacinthi; this method was based on amplification of a subsequence of the type IV fimbrial-subunit gene fimA from strain S148. The fimA gene was amplified by PCR with degenerate DNA primers designed by using the N-terminal and C-terminal amino acid sequences of trypsin fragments of FimA. The nucleotide sequence of fimA was determined and compared with the nucleotide sequences coding for the fimbrial subunits in other type IV fimbria-producing bacteria, such as Xanthomonas campestris pv. vesicatoria, Neisseria gonorrhoeae, and Moraxella bovis. In a PCR internal primers JAAN and JARA, designed by using the nucleotide sequences of the variable central and C-terminal region of fimA, amplified a 226-bp DNA fragment in all X. hyacinthi isolates. This PCR was shown to be pathovar specific, as assessed by testing 71 Xanthomonas pathovars and bacterial isolates belonging to other genera, such as Erwinia and Pseudomonas. Southern hybridization experiments performed with the labelled 226-bp DNA amplicon as a probe suggested that there is only one structural type IV fimbrial-gene cluster in X. hyacinthi. Only two Xanthomonas translucens pathovars cross-reacted weakly in PCR. Primers amplifying a subsequence of the fimA gene of X. campestris pv. vesicatoria (T. Ojanen-Reuhs, N. Kalkkinen, B. Westerlund-Wikström, J. van Doorn, K. Haahtela, E.-L. Nurmiaho-Lassila, K. Wengelink, U. Bonas, and T. K. Korhonen, J. Bacteriol. 179: 1280–1290, 1997) were shown to be pathovar specific, indicating that the fimbrial-subunit sequences are more generally applicable in xanthomonads for detection purposes. Under laboratory conditions, approximately 1,000 CFU of X. hyacinthi per ml could be detected. In inoculated leaves of hyacinths the threshold was 5,000 CFU/ml. The results indicated that infected hyacinths with early symptoms could be successfully screened for X. hyacinthi with PCR. PMID:11157222

  10. The member of the Academy H.P. Keres and the Relativity theory in Estonia

    NASA Astrophysics Data System (ADS)

    Kuusk, P.; Muursepp, P. V.; Piir, Ivar

    1987-10-01

    The first popular lecture on the Einstein theory of relativity was given in Estonia already in 1914 by Jaan Sarv (1877-1954)[1],afterwards a professor of mathematics at the Tartu University. The first student courses on special relativity were delivered by Professor of Mathematics Juri Nuut (1892-1952): non-Euclidean geometry (1930), the mathematical theory of relativity (1932/1933),the Lorenz transformations (1937). His own research work concerned the Lobachevsky geometry [7] and its application to cosmology [6]. Harald Keres qraguated from the Tartu University in 1936. He gave the first student course on general relativity (based on books [11-14]in 1940.In 1942,he got the dr.phil.nat degree form the Tartu University for his theses "Raum und Zeit in der allgemeinen Relativitatstheorie". The degree of the doctor of mathematical and physical sciences was confirmed by VAK (the All-Union Higher Attestation Commission) in 1949.In this period, he got aquainted with the leading Soviet scientists working on General Relativity, prof.V.A.Fock,Prof.D.D.Ivanenko,Prof.A.Z.Petrov,and Prof.M.F.Shirokov. After World War two all-union university courses were introduced in Tartu State University. According to the curriculum of the course the special theory of relativity is a part of electrodynamics obligatory for all students of the department of Physics. From 1947 till 1985 this course was delivered by Prof.PaulKard(1914-1985).He also published a number of text-books on the subject [15-19]. The general theory of relativity was read by Prof.H.Keres in 1951-1960 and later by his pupils R.Lias and A.Koppel [20-23] as a special course for students specializing in theoretical Physics. The first PHD-s in general relativity were made by R.Lias [27](1954) and I.Piir [28] (1955). In 1961, Prof.H.Keres was elected a member of the Academy of Sciences of the Estonian S.S.R. He left the TArtu State University and began to work in the Institute of Physics as the head of the Department of

  11. Introduction

    NASA Astrophysics Data System (ADS)

    Narlikar, J. V.; Sathyaprakash, B. S.

    2014-03-01

    The ICGC Meetings: 1987-2011 When India became an independent nation in 1947, the presence of Jawaharlal Nehru on the scene, as the Prime Minister was a fortunate circumstance. For, Nehru was a visionary, who believed that the future of the new nation should be guided by science and technology (S & T), and so with like-minded scientists like, Shanti Swarup Bhatnagar, Homi Bhabha, Meghnad Saha, and Daulatsingh Kothari in leading positions, Nehru set about creating an extensive infrastructure for S & T. The initiatives taken in and around 1947 began to yield dividends in a couple of decades, and by the late 60s and early 70s, major S & T organizations and associated trained human resources were making significant contributions to the country's development, both material and intellectual. Amongst these may be included, the creation of various scientific societies devoted to specific subjects. These came in response to the urge of scientists to meet as a group for discussions in their fields of research. So, it was in 1969, a number of research workers in the field of general relativity and gravitation (GRG), who had gathered for a workshop in Ahmedabad, resolved to form a society for GRG. The initiative was taken by P C Vaidya, who pointed out the advantages of forming such a recognized group, mentioning that the international community of workers in GRG had already formed such a society. The Indian Association for General Relativity and Gravitation (IAGRG), thus, came up in 1969 with the veteran relativist V V Narlikar, as its first President. Some three years later, the astronomical community responding to a similar urge, formed the Astronomical Society of India (ASI), under the presidency of Vainu Bappu, the Founder Director of the Indian Institute of Astrophysics, Bangalore. Since the days of discovery of quasars in 1963, there has been an alliance between gravitation theorists and astrophysicists, resulting in the Texas Symposia, which are held once every two