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    51. Completeness
    ... This set includes probable giant branch stars which can most clearly be seen in Figure 7 as a group of stars near V = 14 and R - I = 0.5 which lie in between the background and the PMS stars. ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/~swolk/thesis/optical/node9.html -- 6.6 Кб -- 02.10.2012
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    52. Spectroscopic Data
    ... The spectral types of the target stars were determined by comparing source line ratios to those of standard stars. ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/~swolk/thesis/optical/node7.html -- 7.0 Кб -- 02.10.2012
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    53. The AstroStat Slog upper limit
    ... I rather skip all technical details on ultracool dwarfs and binary stars, reviews on star formation studies, like initial mass function (IMF), astronomical survey studies, which Allen gave a fair explanation in arxiv/astro-ph:0707.2064v1 but want to ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/AstroStat/slog/groundtruth.info/AstroStat/slog/tag/upper-limit/index.html -- 25.6 Кб -- 01.03.2014
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    54. Contents
    ... Next: List of Figures Up: Watching the Stars go Previous: Watching the Stars go . Introduction . X--ray Activity and PMS Stars. ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/~swolk/thesis/node1.html -- 11.6 Кб -- 01.10.2012
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    55. Pat Slane: Research
    ... Neutron star work includes studies of their cooling properties to provide constraints on the physics of matter at ultrahigh density, the structure and evolution of the wind nebulae produced by pulsars, and the demographics of the young neutron star ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/~slane/PSlane/Research.html -- 33.9 Кб -- 03.02.2013
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    56. Chandra Images for SNR J0059.4-7210
    ... Chandra Spectrum for SNR J0059.4-7210 . ObsID 1881 . all diffuse . diffuse around star . star. ... ObsID 1881 . all diffuse . diffuse around star . star. ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/ChandraSNR/SNRJ0059.4-7210/chandra_spectra.cgi -- 4.5 Кб -- 03.02.2013
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    57. Conclusions
    ... stars in Orion OB1a and OB1b, I hoped to gather some insights to the evolution of ... showed that the Orion OB1b stars are about 0.5 dex older than the Orion OB1a stars ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/~swolk/thesis/conclusions/node1.html -- 10.7 Кб -- 02.10.2012
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    58. http://hea-www.harvard.edu/CHAMP/EDUCATION/PUBLIC/whitedwarfs_pics.html
    ... star) has somehow thrown off gas to form the planetary nebula that surrounds the star ... so much gas accumulated onto the star that the star just exploded causing the gas to ...
    [ Сохраненная копия ]  Ссылки http://hea-www.harvard.edu/CHAMP/EDUCATION/PUBLIC/whitedwarfs_pics.html -- 4.3 Кб -- 02.10.2012
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    59. http://hea-www.harvard.edu/~pgreen/educ/Web_Reading_Quiz.doc
    ... older, metal-poor stars are blue. d) ? the hottest stars are the oldest stars in a cluster. Your NAME (required for credit!) ...
    [ Текст ]  Ссылки http://hea-www.harvard.edu/~pgreen/educ/Web_Reading_Quiz.doc -- 31.0 Кб -- 05.04.2002
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    60. http://hea-www.harvard.edu/~pgreen/educ/Web_Reading_Quiz2.doc
    ... 31 Feb, 2007 Giant stars are rare because a) they do not form as often as main sequence stars. b) giant stars are unstable. c ...
    [ Текст ]  Ссылки http://hea-www.harvard.edu/~pgreen/educ/Web_Reading_Quiz2.doc -- 10.0 Кб -- 05.04.2002
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