Rho Cassiopeiae

Rho Cassiopeiae

Location of Rho Cassiopeiae in the Cassiopeia constellation.
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia
Right ascension 23h 54m 23.0s[1]
Declination +57° 29′ 58″[1]
Apparent magnitude (V) 4.1 to 6.2[2]
Characteristics
Spectral type G2Iae[3] (F8pIa-K0pIa-0)[2]
U−B color index 1.15[4]
B−V color index 1.26[4]
Variable type semiregular (SRD)[2]
Astrometry
Radial velocity (Rv)−47[3] km/s
Proper motion (μ) RA: −4.54[1] mas/yr
Dec.: −3.45[1] mas/yr
Parallax (π)0.28 ± 0.58[1] mas
Distance2,500[5] pc
Absolute magnitude (MV)–9.5[6]
Details
Mass14-30[7] M☉
Radius400-500[6] R☉
Luminosity~500,000[6] L☉
Surface gravity (log g)0.1[3] cgs
Temperature5777-7200[3][6] K
Metallicity [Fe/H]0.3[8] dex
Rotational velocity (v sin i)25[9] km/s
Other designations
7 Cassiopeiae, HR 9045, BD+56°3111, HD 224014, SAO 35879, FK5 899, HIP 117863, GC 33160
Database references
SIMBADdata

Rho Cassiopeiae (/ˌroʊ kæsiəˈpiː.iː/; ρ Cas, ρ Cassiopeiae) is a yellow hypergiant star in the constellation Cassiopeia. It is about 8,200 light-years (2,500 pc) from Earth, yet can still be seen by the naked eye as it is 500,000 times brighter than the Sun. On average it has an absolute magnitude of −9.5, making it visually one of the brightest stars known. Its diameter measures 450 times that of the Sun, approximately 630,000,000 kilometers, or about twice the size of the Earth's orbit.

Rho Cassiopeiae is a single star, and is categorized as a semiregular variable. As a yellow hypergiant, it is one of the rarest types of stars. Only around a dozen are known in the Milky Way, but it is not the only one in its constellation which also contains V509 Cassiopeiae.[10]

Observation

Visual light curve for Rho Cas from 1933 - 2015

The Bayer designation for this star was established in 1603 as part of the Uranometria, a star catalog produced by Johann Bayer. The star catalog by John Flamsteed published in 1712, which orders the stars in each constellation by their right ascension, gave this star the Flamsteed designation 7 Cassiopeiae.

Rho Cas was first described as variable in 1901. It was classified only as "pec." with a small but definite range of variation.[11] Its nature continued to be unclear during the deep visual minimum in 1946, although it was presumed to be related to the detection of an expanding shell around the star. The spectrum developed lower excitation features described as typical of an M star rather than the previous F8 class.[12] The nature of Rho Cas was eventually clarified as a massive luminous unstable star, pulsating and losing mass, and occasionally becoming obscured by strong bouts of mass loss.[13]

Rho Cas usually has an apparent magnitude near 4.5, but in 1946 it unexpectedly dimmed to 6th magnitude and cooled by over 3,000 Kelvin, before returning to its previous brightness. A similar eruption was recorded in 1893, suggesting that it undergoes these eruptions approximately once every 50 years.[14] This happened again in 2000–2001, when it was observed by the William Herschel Telescope.[14]

Properties

From left to right: the Sun (1 R☉ - not visible in this thumbnail), the Pistol Star (340 R☉), Rho Cassiopeiae (450 R☉), Betelgeuse (1000 R☉) and VY Canis Majoris (1420 R☉). The orbits of Jupiter (5.23 AU) and Neptune (30.01 AU) are included for comparison.

Rho Cassiopeiae is one of the most luminous yellow stars known. It is close to the Eddington luminosity limit and normally loses mass at around 10-6 M☉/yr, hundreds of millions of times the rate of the solar wind. Much of the time it has a temperature over 7,000K, a radius around 400 R☉, and pulsates irregularly producing small changes in brightness. Approximately every 50 years it undergoes a larger outburst and blows off a substantial fraction of its atmosphere, causing the temperature to drop around 1,500K and the brightness to drop by up to 1.5 magnitudes. In 2000–2001 the mass loss rate jumped to 5×10-2 M☉/yr, ejecting in total approximately 3% of a solar mass or 10,000 Earth masses.[9][14] The luminosity remains roughly constant during the outbursts at half a million L☉, but the radiation output shifts towards the infra red.

Surface abundances of most heavy elements on Rho Cas are enhanced relative to the Sun, but carbon and oxygen are depleted. This is expected for a massive star where hydrogen fusion takes place predominantly via the CNO cycle. In addition to the expected helium and nitrogen convected to the surface, sodium is strongly enhanced, indicating that the star had experienced a dredge-up while in a red supergiant stage. Therefore it is expected that Rho Cas is now evolving towards hotter temperatures. It is currently core helium burning through the triple alpha process.[8]

The relatively low mass and high luminosity of a post-red supergiant star is a source of instability, pushing it close to the Eddington Limit. However, yellow hypergiants lie in a temperature range where opacity variations in zones of partial ionisation of hydrogen and helium cause pulsations, similar to the cause of Cepheid variable pulsations. In hypergiants, these pulsations are generally irregular and small, but combined with the overall instability of the outer layers of the star they can result in larger outbursts. This may all be part of an evolutionary trend towards hotter temperatures through the loss of the star's atmosphere.[8]

Naming

ρ Cassiopeiae is a member of the Chinese constellation Flying Serpent 螣蛇 (Téng Shé), in the Encampment mansion. In order, the 22 member stars are α and 4 Lacertae, π2 and π1 Cygni, stars 5 and 6, HD 206267, 13 and ε Cephei, β Lacertae, σ, ρ, τ, and AR Cassiopeiae, 9 Lacertae, 3, 7, 8, λ, ψ, κ, and ι Andromedae. Consequently, ρ Cassiopeiae is known as 螣蛇十二 (Téng Shé shíèr, English: the Twelfth Star of Flying Serpent)[15]

References

  1. 1 2 3 4 5 Van Leeuwen, F. (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.
  2. 1 2 3 "GCVS Query=Rho Cas". General Catalogue of Variable Stars @ Sternberg Astronomical Institute, Moscow, Russia. Retrieved 2010-11-24.
  3. 1 2 3 4 Klochkova, V. G.; Panchuk, V. E.; Tavolganskaya, N. S.; Usenko, I. A. (2013). "Instability of the kinematic state in the atmosphere of the hypergiant Rho Cas outside outburst". Astronomy Reports 58 (2): 101–111. arXiv:1312.6922v1. Bibcode:2014ARep...58..101K. doi:10.1134/S1063772913120044.
  4. 1 2 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues 2237: 0. Bibcode:2002yCat.2237....0D.
  5. ↑ Jura, M.; Kleinmann, S. G. (1990). "The probable dust formation episode around Rho Cassiopeiae". The Astrophysical Journal 351: 583. Bibcode:1990ApJ...351..583J. doi:10.1086/168496.
  6. 1 2 3 4 Gorlova, N.; Lobel, A.; Burgasser, A. J.; Rieke, G. H.; Ilyin, I.; Stauffer, J. R. (2006). "On the CO Near‐Infrared Band and the Line‐splitting Phenomenon in the Yellow Hypergiant ρ Cassiopeiae". The Astrophysical Journal 651 (2): 1130–1150. arXiv:astro-ph/0607158. Bibcode:2006ApJ...651.1130G. doi:10.1086/507590.
  7. ↑ Gesicki, K. (1992). "A Modelling of Circumstellar BAII Lines for the Hypergiant Rho-Cassiopeiae". Astronomy and Astrophysics 254: 280. Bibcode:1992A&A...254..280G.
  8. 1 2 3 Israelian, G.; Lobel, A.; De Jager, C.; Musaev, F. (1998). "The Variable Spectrum of the Yellow Hypergiant rho Cassiopeiae". ASP Conf. Ser. 154: 1601. Bibcode:1998ASPC..154.1601I.
  9. 1 2 Lobel, A.; Israelian, G.; De Jager, C.; Musaev, F.; Parker, J. Wm.; Mavrogiorgou, A. (1998). "The spectral variability of the cool hypergiant rho Cassiopeiae". Astronomy and Astrophysics 330: 659. Bibcode:1998A&A...330..659L.
  10. ↑ Israelian, G.; Lobel, A.; Schmidt, M. R. (1999). "The Yellow Hypergiants HR 8752 and ρ Cassiopeiae near the Evolutionary Border of Instability". The Astrophysical Journal 523 (2): L145. arXiv:astro-ph/9908308. Bibcode:1999ApJ...523L.145I. doi:10.1086/312283.
  11. ↑ Pickering, E. C.; Colson, H. R.; Fleming, W. P.; Wells, L. D. (1901). "Sixty-four new variable stars". Astrophysical Journal 13: 226. Bibcode:1901ApJ....13..226P. doi:10.1086/140808.
  12. ↑ Beardsley, Wallace R. (1953). "The spectrum of ρ Cassiopeiae". Astronomical Journal 58: 34. Bibcode:1953AJ.....58...34B. doi:10.1086/106807.
  13. ↑ Sheffer, Yaron; Lambert, David L. (1986). "Spectroscopic observations of yellow supergiants. I - Radial pulsations of Rho Cassiopeiae". Publications of the Astronomical Society of the Pacific 98: 914. Bibcode:1986PASP...98..914S. doi:10.1086/131844.
  14. 1 2 3 Lobel, A.; Dupree, A. K.; Stefanik, R. P.; Torres, G.; Israelian, G.; Morrison, N.; De Jager, C.; Nieuwenhuijzen, H.; Ilyin, I.; Musaev, F. (2003). "High‐Resolution Spectroscopy of the Yellow Hypergiant ρ Cassiopeiae from 1993 through the Outburst of 2000–2001". The Astrophysical Journal 583 (2): 923–954. arXiv:astro-ph/0301238. Bibcode:2003ApJ...583..923L. doi:10.1086/345503.
  15. ↑ 陳輝樺 (Chen Huihua), ed. (7 July 2006). "Activities of Exhibition and Education in Astronomy" 天文教育資訊網 (in Chinese). Retrieved 10 June 2015.

External links

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