Wikipedia

PZ Cassiopeiae

PZ Cassiopeiae is a red supergiant star located in the constellation of Cassiopeia, and a semi-regular variable star.

PZ Cassiopeiae

PZ Cassiopeiae is the bright star towards the upper right in this WISE infrared image.
Observation data
Epoch J2000      Equinox J2000
Constellation Cassiopeia
Right ascension 23h 44m 03.28104s[1]
Declination 61° 47′ 22.1823″[1]
Apparent magnitude (V) 8.2 – 10.2[2]
Characteristics
Evolutionary stage Red supergiant
Spectral type M3Iab[3]
U−B color index 1.32[4]
B−V color index 2.58[4]
Variable type SRc[5] Cepheid[6]
Astrometry
Radial velocity (Rv)–45.68[7] km/s
Proper motion (μ) RA: −4.15[1] mas/yr
Dec.: −3.55[1] mas/yr
Parallax (π)0.356 ± 0.026 mas[8]
Distance2,810 220
−190[8] pc
Absolute magnitude (MV)−7.89[9]
Details
Mass20 or 25 (initial mass)[8] M☉
Radius1,259—1,336,[8][a] 1,231[10] R☉
Luminosity229,000,[11]
(240,000 – 270,000[8]) L☉
Surface gravity (log g)−0.5[9] cgs
Temperature3,605[3] K
Age8 or 10[8] Myr
Other designations
PZ Cas, IRC  60417, HIP 117078, BD 60°2613, RAFGL 3138
Database references
SIMBADdata

Characteristics

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PZ Cassiopeiae is a luminous red supergiant star, one of the largest stars currently known with a radius over 1,200 times the Sun's radius (R☉), and also one of the most luminous of its type, around 240,000 times more luminous than the Sun (L☉).[10] It is likely to be part of the Cas OB5 stellar association although apparently much younger than the other stars in the association.[8] The star is losing mass at around 2.6×10−5 M☉ per year and has also once been described as a hypergiant.[12][13]

Its distance from Earth was initially estimated to be around 7,800 light-years (2.4 kiloparsecs). Subsequent studies of the star using the water masers that surround it have allowed to refine both the distance and the parameters of this star, deriving an accurate parallax of 0.356±0.026 mas, corresponding to a distance of 9,160 light-years (2.81 kiloparsecs), that translates a luminosity for it around 229,000 L☉, and an initial mass of 20 to 25 times that of the Sun. These parameters are all similar to those estimated for the red hypergiant VY Canis Majoris.[8][11]

A Gaia Data Release 2 parallax of 0.42±0.09 mas gives the star a luminosity below 180,000 L☉ with a corresponding radius of 1,062 R☉.[14]

 
A visual band light curve of PZ Cassiopeiae, from AAVSO data[15]

PZ Cas is a slow semi-regular variable star with the period quoted as 925 days in the General Catalogue of Variable Stars,[16] although periods of 850 and 3,195 days have been derived.[5][2] The visual range is approximate magnitude 8–10, large for this type of variable.[2]

Supergiant or AGB star

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PZ Cas has traditionally been treated as a massive supergiant, comparable to others such as VY CMa, but there is some evidence that it is a possible less massive O-rich S- or SC-type Asymptotic Giant Branch (AGB) or post-AGB star. It shows enrichment of Zr and Ba, but not Li as would be expected for a true supergiant.[17]

Companion

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PZ Cas has a Cepheid variable companion, a 13th magnitude star 12" away.[6]

Notes

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  1. ^ Applying the Stefan–Boltzmann law with a nominal solar effective temperature of 5,772 K:
     .
     .

References

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  1. ^ a b c d 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. S2CID 18759600.
  2. ^ a b c Kiss, L. L.; Szabó, G. M.; Bedding, T. R. (2006). "Variability in red supergiant stars: Pulsations, long secondary periods and convection noise". Monthly Notices of the Royal Astronomical Society. 372 (4): 1721–1734. arXiv:astro-ph/0608438. Bibcode:2006MNRAS.372.1721K. doi:10.1111/j.1365-2966.2006.10973.x. S2CID 5203133.
  3. ^ a b Verhoelst, T.; Zypen, N. Van der; Hony, S.; Decin, L.; Cami, J.; Eriksson, K. (1 April 2009). "The dust condensation sequence in red supergiant stars". Astronomy & Astrophysics. 498 (1): 127–138. arXiv:0901.1262. Bibcode:2009A&A...498..127V. doi:10.1051/0004-6361/20079063. ISSN 0004-6361.
  4. ^ a b 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. Bibcode:2002yCat.2237....0D.
  5. ^ a b Le Squeren, A. M.; Sivagnanam, P.; Dennefeld, M.; David, P. (1992). "A Complete Survey of OH / Infrared Objects from the IRAS LRS Sources Within a Domain of the Color Diagram". Astronomy and Astrophysics. 254: 133. Bibcode:1992A&A...254..133L.
  6. ^ a b Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal. 122 (6): 3466. Bibcode:2001AJ....122.3466M. doi:10.1086/323920.
  7. ^ Famaey, B.; Jorissen, A.; Luri, X.; Mayor, M.; Udry, S.; Dejonghe, H.; Turon, C. (2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430: 165. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  8. ^ a b c d e f g h Kusuno, K.; Asaki, Y.; Imai, H.; Oyama, T. (2013). "Distance and Proper Motion Measurement of the Red Supergiant, Pz Cas, in Very Long Baseline Interferometry H2O Maser Astrometry". The Astrophysical Journal. 774 (2): 107. arXiv:1308.3580. Bibcode:2013ApJ...774..107K. doi:10.1088/0004-637X/774/2/107. S2CID 118867155.
  9. ^ a b Levesque, E. M.; Massey, P.; Olsen, K. A. G.; Plez, B.; Josselin, E.; Maeder, A.; Meynet, G. (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not as Cool as We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv:astro-ph/0504337. Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID 15109583.
  10. ^ a b Healy, Sarah; Horiuchi, Shunsaku; Molla, Marta Colomer; Milisavljevic, Dan; Tseng, Jeff; Bergin, Faith; Weil, Kathryn; Tanaka, Masaomi (23 March 2024). "Red Supergiant Candidates for Multimessenger Monitoring of the Next Galactic Supernova". Monthly Notices of the Royal Astronomical Society. 529 (4): 3630–3650. arXiv:2307.08785. doi:10.1093/mnras/stae738. ISSN 0035-8711.
  11. ^ a b Davies, Ben; Beasor, Emma R. (March 2020). "The 'red supergiant problem': the upper luminosity boundary of Type II supernova progenitors". MNRAS. 493 (1): 468–476. arXiv:2001.06020. Bibcode:2020MNRAS.493..468D. doi:10.1093/mnras/staa174. S2CID 210714093.
  12. ^ Mauron, N.; Josselin, E. (2011). "The mass-loss rates of red supergiants and the de Jager prescription". Astronomy and Astrophysics. 526: A156. arXiv:1010.5369. Bibcode:2011A&A...526A.156M. doi:10.1051/0004-6361/201013993. S2CID 119276502.
  13. ^ Stickland, D. J. (1985). "IRAS observations of the cool galactic hypergiants". The Observatory. 105: 229. Bibcode:1985Obs...105..229S.
  14. ^ Messineo, M.; Brown, A. G. A. (2019). "A Catalog of Known Galactic K-M Stars of Class I Candidate Red Supergiants in Gaia DR2". The Astronomical Journal. 158 (1): 20. arXiv:1905.03744. Bibcode:2019AJ....158...20M. doi:10.3847/1538-3881/ab1cbd. S2CID 148571616.
  15. ^ "Download Data". aavso.org. AAVSO. Retrieved 1 October 2021.
  16. ^ Samus, N. N.; Durlevich, O. V.; et al. (2009). "VizieR Online Data Catalog: General Catalogue of Variable Stars (Samus 2007-2013)". VizieR On-line Data Catalog: B/GCVS. Originally Published in: 2009yCat....102025S. 1. Bibcode:2009yCat....102025S.
  17. ^ García-Hernández, D. A.; García-Lario, P.; Plez, B.; Manchado, A.; d'Antona, F.; Lub, J.; Habing, H. (2007). "Lithium and zirconium abundances in massive Galactic O-rich AGB stars". Astronomy and Astrophysics. 462 (2): 711. arXiv:astro-ph/0609106. Bibcode:2007A&A...462..711G. doi:10.1051/0004-6361:20065785. S2CID 16016698.
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