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RS Persei is a red supergiant variable star located in the
RS Persei is classified as a semiregular variable star, with its brightness varying from magnitude 7.82 to 10.0 over 245 days, Detailed studies show that it also pulsates with a long secondary period of days.
Light curve
VSX entry
{{DEFAULTSORT:RS Persei M-type supergiants Perseus (constellation) Persei, RS 014488 BD+56 583 Semiregular variable stars J02222428+5706340
Double Cluster
The Double Cluster (also known as Caldwell 14) consists of the open clusters NGC 869 and NGC 884 (often designated h Persei and χ (chi) Persei, respectively), which are close together in the constellation Perseus. Both visible with t ...
in Perseus
In Greek mythology, Perseus (Help:IPA/English, /ˈpɜːrsiəs, -sjuːs/; Greek language, Greek: Περσεύς, Romanization of Greek, translit. Perseús) is the legendary founder of Mycenae and of the Perseid dynasty. He was, alongside Cadmus ...
. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye.
Location
RS Persei is a member of the clusterNGC 884
NGC 884 (also known as χ Persei) is an open cluster located 7640 light years away in the constellation of Perseus. It is the easternmost of the Double Cluster with NGC 869. NGC 869 and 884 are often designated h and χ Persei, respectively.Som ...
, χ Persei, one half of the famous Double Cluster
The Double Cluster (also known as Caldwell 14) consists of the open clusters NGC 869 and NGC 884 (often designated h Persei and χ (chi) Persei, respectively), which are close together in the constellation Perseus. Both visible with t ...
.
Variability
RS Persei is classified as a semiregular variable star, with its brightness varying from magnitude 7.82 to 10.0 over 245 days, Detailed studies show that it also pulsates with a long secondary period of days.
Properties
RS Persei is a large cool star with a temperature of 3,500 K. This makes it luminous, although much of its radiation is emitted in the infrared. In 2005, RS Per was calculated to have a bolometric luminosity of and a radius around . More recently, 2014 calculations across all wavelengths gives the star a lower luminosity of based on an assumed distance, and a radius of based on the measured angular diameter and luminosity. Even more recent measurements based on itsGaia Data Release 2
The ''Gaia'' catalogues are star catalogues created using the results obtained by ''Gaia'' space telescope.
The catalogues are released in stages that will contain increasing amounts of information; the early releases also miss some stars, especia ...
parallax gives a luminosity below with a corresponding radius of . It is surrounded by dust that has condensed from material lost by the star.
RS Persei has sometimes been considered to be a highly evolved low mass Asymptotic Giant Branch
The asymptotic giant branch (AGB) is a region of the Hertzsprung–Russell diagram populated by evolved cool luminous stars. This is a period of stellar evolution undertaken by all low- to intermediate-mass stars (about 0.5 to 8 solar masses) lat ...
(AGB) star, but calculations of its current mass suggest that it is a low mass supergiant. NGC 244 is also too young to host AGB stars.
References
External links
Light curve
VSX entry
{{DEFAULTSORT:RS Persei M-type supergiants Perseus (constellation) Persei, RS 014488 BD+56 583 Semiregular variable stars J02222428+5706340