In astrophysics, the Phillips relationship is the relationship between the peak luminosity of a Type Ia supernova and the speed of luminosity evolution after maximum light. The relationship was independentlydiscovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. They found that the faster the supernova faded from maximum light, the fainter its peak magnitude was. As a main parameter characterizing the light curve shape, Pskovskii used β, the mean rate of decline in photographic brightness from maximum light to the point at which the luminosity decline rate changes. β ismeasured in magnitudes per 100-day intervals. Selection of this parameter is justified by the fact that, at that time, the probability of disc

Property Value
dbo:abstract
  • 飛利浦關係是天文物理中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。 這種相關性在1993年被M.飛利浦在Calán/托洛洛超新星巡天時再度發現。它已被改寫,其中包括多個光度法的帶通,和相對於標轉範本在時間軸上的擴張'。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天的星等光度曲線,這個參數稱為 ,給出最大光度和實際的B星等關係狀態: (zh)
  • In astrophysics, the Phillips relationship is the relationship between the peak luminosity of a Type Ia supernova and the speed of luminosity evolution after maximum light. The relationship was independentlydiscovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. They found that the faster the supernova faded from maximum light, the fainter its peak magnitude was. As a main parameter characterizing the light curve shape, Pskovskii used β, the mean rate of decline in photographic brightness from maximum light to the point at which the luminosity decline rate changes. β ismeasured in magnitudes per 100-day intervals. Selection of this parameter is justified by the fact that, at that time, the probability of discovering a supernova before the maximum light, and obtain the full light curve, was small. Moreover, the existing light curves were mostly incomplete. On the other hand, to determine the decline after the maximum light was rather simple for most observed supernovae. In the early 1980s CCD cameras appeared, and the number of SNe discoveries increased substantially. Moreover, the probability of discovering SNe before they reached maximum light and following their brightness evolution longer also increased. The first light curves of SNe Ia obtained using CCD photometry showed that some supernovae had faster decline rates than others. Later, the low luminosity SN Ia 1991bg with a fast decline rate was discovered.All this motivated the American astronomer Mark M. Phillips to revise this relationship precisely during the course of the Calán/Tololo Supernova Survey. The correlation had been difficult to prove because Pskovskii's slope (β) parameter was difficult to measure with precision in practice, a necessary condition to prove the correlation. Rather than trying to determine the slope, Phillips used a simpler and more robust procedure that consisted in "measuring the total amount in magnitudes that the light curve decays from its peak brightness during some specified period following maximum light." It was defined as the decline in the B-magnitude light curve from maximum light to the magnitude 15 days after B-maximum, a parameter he called . The relation states that the maximum intrinsic B-band magnitude is given by Phillips dedicated the journal article confirming Yuri Pskovskii's proposed correlation to Pskovskii, who died a few weeks after Phillips' evidence confirming the relationship was published. It has been recast to include the evolution in multiple photometric bandpasses, with a significantly shallower slope and as a stretch in the time axis relative to a standard template.The relation is typically used to bring any Type Ia supernova peak magnitude to a standard candle value. (en)
dbo:thumbnail
dbo:wikiPageID
  • 24551923 (xsd:integer)
dbo:wikiPageRevisionID
  • 737499709 (xsd:integer)
dct:subject
rdf:type
rdfs:comment
  • 飛利浦關係是天文物理中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。 這種相關性在1993年被M.飛利浦在Calán/托洛洛超新星巡天時再度發現。它已被改寫,其中包括多個光度法的帶通,和相對於標轉範本在時間軸上的擴張'。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天的星等光度曲線,這個參數稱為 ,給出最大光度和實際的B星等關係狀態: (zh)
  • In astrophysics, the Phillips relationship is the relationship between the peak luminosity of a Type Ia supernova and the speed of luminosity evolution after maximum light. The relationship was independentlydiscovered by the American statistician and astronomer Bert Woodard Rust and the Soviet astronomer Yury Pavlovich Pskovskii in the 1970s. They found that the faster the supernova faded from maximum light, the fainter its peak magnitude was. As a main parameter characterizing the light curve shape, Pskovskii used β, the mean rate of decline in photographic brightness from maximum light to the point at which the luminosity decline rate changes. β ismeasured in magnitudes per 100-day intervals. Selection of this parameter is justified by the fact that, at that time, the probability of disc (en)
rdfs:label
  • 飛利浦關係 (zh)
  • Phillips relationship (en)
owl:sameAs
prov:wasDerivedFrom
foaf:depiction
foaf:isPrimaryTopicOf
is dbo:wikiPageRedirects of
is foaf:primaryTopic of