查看“︁菲利普斯關係”︁的源代码

'''菲利普斯關係'''是[[天文物理]]中[[Ia超新星]]的亮度峰值和最大亮度之後的光度變化之間的關係。

它最初是由美國天文學家伯特·秀在1974年，和蘇聯天文學家尤里·伯考伏斯基在1977年發現的。他們發現超新星的光度在最大光度過後，衰減的越快它的峰值也越暗淡<ref>{{cite journal | last = Rust | first = B. W. | title = The Use of Supernovae Light Curves for Testing the Expansion Hypothesis and Other Cosmological Relations | journal = [PhD thesis, University of Illinois] | url = http://www.iaea.org/inis/collection/NCLCollectionStore/_Public/06/179/6179223.pdf | access-date = 2015-06-21 | archive-date = 2016-03-04 | archive-url = https://web.archive.org/web/20160304061039/http://www.iaea.org/inis/collection/NCLCollectionStore/_Public/06/179/6179223.pdf | dead-url = no }} {{Wayback|url=http://www.iaea.org/inis/collection/NCLCollectionStore/_Public/06/179/6179223.pdf |date=20160304061039 }}</ref><ref>{{cite journal | last = Pskovskii | first = Yu. P. | title = Light curves, color curves, and expansion velocity of type I supernovae as functions of the rate of brightness decline | journal = [[Astronomy Reports | Soviet Astronomy]] | volume = 21 | pages = 675 | date = 1977 | bibcode = 1977SvA....21..675P}}</ref><ref>{{cite journal | last = Pskovskii | first = Yu. P. | title = Photometric classification and basic parameters of type I supernovae | journal = [[Astronomy Reports | Soviet Astronomy]] | volume = 28 | pages = 658-664 | date = 1984 | bibcode = 1984SvA....28..658P}}</ref>。

這種相關性在1993年被M.菲利普斯在{{link-en|Calán/托洛洛超新星巡天|Calán/Tololo_Survey}}時再度發現<ref>{{cite journal | last = Phillips | first = M. M. | authorlink = Mark M. Phillips | title = The absolute magnitudes of Type IA supernovae | journal = [[Astrophysical Journal|Astrophysical Journal Letters]] | volume = 413 | issue = 2 | pages = L105–L108 | date = 1993 | doi = 10.1086/186970 | bibcode = 1993ApJ...413L.105P}}</ref>。它已被改寫，其中包括多個光度法的帶通<ref>Hamuy, M., Phillips, M. M., Maza, J., Suntzeff, N. B., Schommer, R. A., & Aviles, R. 1995, ''Astronomical Journal'', 109, 1</ref><ref>Riess, A. G., Press, W. H., & Kirshner, R. P. 1996, ''AstrophysicsJournal'', 473, 88</ref>，和相對於標轉範本在時間軸上的''擴張'<ref>Perlmutter, S. A., & et al.  1997, ''NATO ASIC Proc. 486: Thermonuclear Supernovae'', 749</ref>。
這關係通常用於導出Ia超新星最大亮度的[[標準燭光]]值。

它被定義在''B''星等從最大光度至下降15天的[[視星等|星等]][[光度曲線]]，這個參數稱為<math>\Delta{m}_{15}</math>，給出最大光度和實際的B星等關係狀態<ref>{{cite book | author = Rosswog | author2 =Bruggen | title = High Energy Astrophysics | year = 2007 | url = https://archive.org/details/introductiontohi0000ross }}</ref>：

<math> M_\mathrm{max}(B) = -21.726 + 2.698 \Delta m_{15} (B). </math>

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== 參考資料 ==
{{Reflist|30em}}

{{超新星}}

[[Category:天体物理学]]
[[Category:超新星]]