Astro-Physics

Results: 813



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101

Astro 2 van der Veen Spring 2002

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Source URL: web.physics.ucsb.edu

Language: English - Date: 2003-08-09 15:54:56
    102

    SUMMARY IV: FUNDAMENTAL PRINCIPLES • Stars are self-gravitating bodies in dynamical equilibrium → balance of gravity and internal pressure forces (hydrostatic equilibrium); • stars lose energy by radiation from the

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    Source URL: www-astro.physics.ox.ac.uk

    Language: English - Date: 2004-11-18 06:59:04
      103

      3. THE PHYSICAL STATE OF THE STELLAR INTERIOR Fundamental assumptions: (Pc)¯ ∼ 5 × 1014 N m−2

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      Source URL: www-astro.physics.ox.ac.uk

      Language: English - Date: 2004-11-18 06:52:11
        104

        STRUCTURE OF THE SUN HELIOSEISMOLOGY (I) • The Sun is the only star for which we can measure internal properties → test of stellar structure theory

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        Source URL: www-astro.physics.ox.ac.uk

        Language: English - Date: 2003-10-31 06:50:52
          105

          arXiv:astro-phv1 12 SepNew Constraints on ΩM, ΩΛ, and w from an Independent Set of Eleven High-Redshift Supernovae Observed with HST1 R. A. Knop2,3,4 , G. Aldering5,4 , R. Amanullah6 , P. Astier7 , G

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          Source URL: web.physics.ucsb.edu

          Language: English - Date: 2004-07-22 15:14:55
            106

            ASTRO-PHYSICS 900GTOGERMAN EQUATORIAL MOUNT 42° Latitude

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            Source URL: www.astro-physics.com

            Language: English - Date: 2005-10-04 10:23:12
              107

              Page 2 Stellar Structure and Evolution: Syllabus Ph. Podsiadlowski (MTDWB 702, (, ) (www-astro.physics.ox.ac.uk/˜podsi/lec mm03.html)

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              Source URL: www-astro.physics.ox.ac.uk

              Language: English - Date: 2006-10-17 08:40:36
                108

                APPENDICES (Supplementary Material) A. Brown Dwarfs B. Planets C. The CNO Tri-Cycle D. The Structure of the Sun and the Solar Neutrino Problem

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                Source URL: www-astro.physics.ox.ac.uk

                Language: English - Date: 2004-12-01 08:11:07
                  109

                  Evolution of Massive Stars 6.3 EVOLUTION OF MASSIVE STARS (M > ∼ 13 M¯) (CO: 13.3) • massive stars continue to burn nuclear fuel beyond

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                  Source URL: www-astro.physics.ox.ac.uk

                  Language: English - Date: 2004-12-01 08:00:54
                    110

                     (2) low-mass stars: ideal-gas law, Kramer’s opacity law, i.e. ∝ T−zero-age main sequence (ZAMS): homogeneous

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                    Source URL: www-astro.physics.ox.ac.uk

                    Language: English - Date: 2004-11-23 08:50:49
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