| 词条 | RS Persei |
| 释义 |
| name = RS Persei }}{{Starbox image | image = | caption = RS Persei is the red star closest to the centre of NGC 884, the right hand cluster (north is down). }}{{Starbox observe | epoch=J2000 | ra={{RA|2|22|24.288}}[1] | dec={{DEC|+57|0.6|34.08}}[1] | appmag_v=7.82-10.0[2] | constell=Perseus }}{{Starbox character | class=M4Iab[3] | b-v= | u-b= | variable=SRc[2] }}{{Starbox astrometry | radial_v={{val|-38.0|2}}[4] | prop_mo_ra={{val|-0.371|0.137}}[7] | prop_mo_dec={{val|-0.931|0.165}}[7] | parallax=0.6437 | p_error=0.0822 | parallax_footnote=[5] | dist_pc={{val|2,345|55|fmt=commas}}[6] | dist_ly= | absmag_v=−6.18[7] }}{{Starbox detail | source=[6] | mass=12-15 | radius={{val|770|30}} | luminosity={{val|77,600|9,500|8,400|fmt=commas}} | temperature={{val|3,470|90|fmt=commas}} | metal= | rotation= | gravity={{val|-0.2|0.05}} | age= }}{{Starbox catalog | names= RS Per, HD 14488, BD+56°583, 2MASS J02222428+5706340, AAVSO 0215+56A }}{{Starbox reference | Simbad=RS+Persei }}{{Starbox end}} RS Persei is a red supergiant variable star located in the Double Cluster in Perseus. The star's apparent magnitude varies from 7.82 to 10.0, meaning it is never visible to the naked eye. LocationRS Persei is a member of the cluster NGC 884, χ Persei, one half of the famous Double Cluster.[8] VariabilityRS Persei is classified as a semiregular variable star, with its brightness varying from magnitude 7.82 to 10.0 over 245 days,[2] Detailed studies show that it also pulsates with a long secondary period of {{val|4,200|1,500|fmt=commas}} days.[9] PropertiesRS Persei is a large cool star, 3,500 K and with a radius of {{solar radius|770}}. Levesque calculates {{solar radius|1,000}}.[7] This makes it luminous, although much of its radiation is emitted in the infrared. Across all wavelengths it is at least 70,000 times as luminous as the sun. It is surrounded by dust that has condensed from material lost by the star.[10] RS Persei has sometimes been considered to be a highly evolved low mass Asymptotic Giant Branch (AGB) star,[11] but calculations of its current mass suggest that it is a low mass supergiant. NGC 244 is also too young to host AGB stars.[6] References1. ^1 {{cite journal|bibcode=2003yCat.2246....0C|title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)|journal=VizieR On-line Data Catalog: II/246. Originally Published In: 2003y Cat.2246....0C|volume=2246|author1=Cutri|first1=R. M|last2=Skrutskie|first2=M. F|last3=Van Dyk|first3=S|last4=Beichman|first4=C. A|last5=Carpenter|first5=J. M|last6=Chester|first6=T|last7=Cambresy|first7=L|last8=Evans|first8=T|last9=Fowler|first9=J|last10=Gizis|first10=J|last11=Howard|first11=E|last12=Huchra|first12=J|last13=Jarrett|first13=T|last14=Kopan|first14=E. L|last15=Kirkpatrick|first15=J. D|last16=Light|first16=R. M|last17=Marsh|first17=K. 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7 : M-type supergiants|Perseus (constellation)|Objects with variable star designations|Henry Draper Catalogue objects|Durchmusterung objects|Semiregular variable stars|2MASS objects |
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