Rho Persei

Rho Persei (Rho Per, ρ Persei, ρ Per) is a star in the northern constellation of Perseus. It has the traditional name Gorgonea Tertia /ɡɔːrɡəˈniːə ˈtɜːrʃə/,[11] being the third member of the quartet called the Gorgonea in reference to the Gorgons from the legend of Perseus.[9] An apparent visual magnitude of +3.39[2] makes it visible to the naked eye, but a challenge to view from a well-lit urban environment. Based upon parallax measurements, it is located at a distance of roughly 308 light-years (94 pc) from Earth.[1]

ρ Persei
Location of ρ Persei (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Perseus
Right ascension  03h 05m 10.59385s[1]
Declination +38° 50′ 24.9943″[1]
Apparent magnitude (V) +3.39[2]
Characteristics
Evolutionary stage asymptotic giant branch[3]
Spectral type M4 II[4]
U−B color index +1.79[2]
B−V color index +1.65[2]
Variable type SRb[4]
Astrometry
Radial velocity (Rv)+29.10 ± 0.30[5] km/s
Proper motion (μ) RA: +129.22[1] mas/yr
Dec.: –105.70[1] mas/yr
Parallax (π)10.60 ± 0.25[1] mas
Distance308 ± 7 ly
(94 ± 2 pc)
Absolute magnitude (MV)–1.7[6]
Details
Mass5.0[7] M☉
Radius150[7] R☉
Luminosity2,290[7] L☉
Surface gravity (log g)1.0[8] cgs
Temperature4,111[8] K
Rotational velocity (v sin i)11.2[8] km/s
Age4.4 × 108[9] years
Other designations
Gorgonea Tertia, ρ Persei, 25 Per, BD+38°630, FK5 109, GC 3682, HD 19058, HIP 14354, HR 921, PPM 68074, SAO 56138.[10]
Database references
SIMBADdata

Rho Persei is a semiregular variable star, whose apparent magnitude varies between 3.3 and 4.0[12] with periods of 50, 120 and 250 days.[6] The star has reached the asymptotic giant branch of its evolution.[3] It is a bright giant star with a stellar classification of M4 II.[4] The outer envelope has an effective temperature of 4,111 K,[8] giving it the red-orange hue of an M-type star.[13]

This star has a mass five times the mass of the Sun, while its radius has expanded to 150 times solar. It is radiating some 2,290 times the Sun's luminosity. Rho Persei is losing mass at the rate of 1.2 × 10−8 solar masses per year, or the equivalent of the Sun's mass every 83 million years.[7] It is about 440 million years in age.[9]

Naming

In Chinese, 大陵 (Dà Líng), meaning Mausoleum, refers to an asterism consisting of ρ Persei, 9 Persei, τ Persei, ι Persei, κ Persei, β Persei, 16 Persei and 12 Persei. Consequently, the Chinese name for ρ Persei itself is 大陵六 (Dà Líng liù, English: the Sixth Star of Mausoleum.).[14]

gollark: It means "triangular".
gollark: That too.
gollark: No, considered controversial or NSFW *by me*.
gollark: I should really try and figure out how to ban you for when you inevitably do this more.
gollark: I mean, in the metaphorical sense.

References
  1. van Leeuwen, F. (November 2007), "Validation of the new Hipparcos reduction", Astronomy and Astrophysics, 474 (2): 653–664, arXiv:0708.1752, Bibcode:2007A&A...474..653V, doi:10.1051/0004-6361:20078357, S2CID 18759600
  2. Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N
  3. Eggen, Olin J. (July 1992), "Asymptotic giant branch stars near the sun", Astronomical Journal, 104 (1): 275–313, Bibcode:1992AJ....104..275E, doi:10.1086/116239.
  4. Ragland, S.; et al. (November 2006), "First Surface-resolved Results with the Infrared Optical Telescope Array Imaging Interferometer: Detection of Asymmetries in Asymptotic Giant Branch Stars", The Astrophysical Journal, 652 (1): 650–660, arXiv:astro-ph/0607156, Bibcode:2006ApJ...652..650R, doi:10.1086/507453
  5. Famaey, B.; et al. (May 2009), "Spectroscopic binaries among Hipparcos M giants. I. Data, orbits, and intrinsic variations", Astronomy and Astrophysics, 498 (2): 627–640, arXiv:0901.0934, Bibcode:2009A&A...498..627F, doi:10.1051/0004-6361/200810698, S2CID 18739721
  6. Yeşilyaprak, C.; Aslan, Z. (December 2004), "Period-luminosity relation for M-type semiregular variables from Hipparcos parallaxes", Monthly Notices of the Royal Astronomical Society, 355 (2): 601–607, Bibcode:2004MNRAS.355..601Y, doi:10.1111/j.1365-2966.2004.08344.x
  7. Cox, Arthur N.; Becker, Stephen A.; Pesnell, W. Dean (2000), "Chapter 20. Theoretical Stellar Evolution" (PDF), Allen's astrophysical quantities (4th ed.), New York: Springer, p. 516, ISBN 0-387-98746-0, retrieved 2012-01-25 See table 20.5
  8. Massarotti, Alessandro; et al. (January 2008), "Rotational and Radial Velocities for a Sample of 761 HIPPARCOS Giants and the Role of Binarity", The Astronomical Journal, 135 (1): 209–231, Bibcode:2008AJ....135..209M, doi:10.1088/0004-6256/135/1/209
  9. Kaler, James B., "GORGONEA TERTIA (Rho Persei)", Stars, University of Illinois, retrieved 2012-01-25
  10. "rho Per -- Semi-regular pulsating Star", SIMBAD, Centre de Données astronomiques de Strasbourg, retrieved 2012-01-24
  11. Allen, Richard Hinckley (1899), "Star-names and their meanings", New York, G. E. Stechert: 334, Bibcode:1899sntm.book.....A
  12. Kukarkin, B. V.; et al. (1971). "General Catalogue of Variable Stars". General Catalogue of Variable Stars (3rd ed.). Bibcode:1971GCVS3.C......0K. |contribution= ignored (help)
  13. "The Colour of Stars", Australia Telescope, Outreach and Education, Commonwealth Scientific and Industrial Research Organisation, December 21, 2004, retrieved 2012-01-16
  14. (in Chinese) AEEA (Activities of Exhibition and Education in Astronomy) 天文教育資訊網 2006 年 7 月 11 日
This article is issued from Wikipedia. The text is licensed under Creative Commons - Attribution - Sharealike. Additional terms may apply for the media files.