Astronomy:XX Persei

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Short description: Star in the constellation Perseus
XX Persei
Comet Lovejoy.jpg
Red circle.svg
XX Persei (circled) near the Double Cluster and Comet Lovejoy
Credit: Juan lacruz
Observation data
Equinox J2000.0]] (ICRS)
Constellation Perseus
Right ascension  02h 03m 09.35854s[1]
Declination 55° 13′ 56.6229″[1]
Apparent magnitude (V) 7.9 - 9.0[2]
Characteristics
Spectral type M4Ib + B7V[3]
Variable type SRc[4]
Astrometry
Proper motion (μ) RA: −1.263[1] mas/yr
Dec.: −1.819[1] mas/yr
Parallax (π)0.3980 ± 0.0316[1] mas
Distance8,200 ± 700 ly
(2,500 ± 200 pc)
Absolute magnitude (MV)−4.6[5]
Details
Mass16[5] M☉
Radius548[6] - 681[7] R☉
Luminosity42,000[6] L☉
Temperature3,535±170[6] K
Other designations
XX Per, BD+54°444, GSC 03689-01837, HD 12401, HIP 9582, IRC+50052, 2MASS J02030935+5513566, HV 3414, SAO 22875, AAVSO 0156+54
Database references
SIMBADdata

XX Persei (IRC +50052 / HIP 9582 / BD+54°444) is a semiregular variable red supergiant star in the constellation Perseus, between the Double Cluster and the border with Andromeda.

Variability

A visual band light curve for XX Persei, plotted from ASAS-SN data[8]

XX Persei is a semiregular variable star of sub-type SRc, indicating a cool supergiant. The General Catalogue of Variable Stars gives the period as 415 days.[4] It also shows a long secondary period which was originally given at 4,100 days.[5] A more recent study shows only slow variations with a period of 3,150 ± 1,000 days.[2] Another study failed to find any long period up to 10,000 days.[9]

Distance

The most likely distance of XX Per is 2,290 pc, from assumed membership of the Perseus OB1 association.[10] Gaia Data Release 3 includes a parallax of 0.3980±0.0316 mas, corresponding to a distance of around 2,500 pc.[1]

Characteristics

XX Per is a red supergiant of spectral type M4Ib with an effective temperature below 4,000 K. It has a large infrared excess, indicating surrounding dust at a temperature of 900 K, but no masers have been detected.[11][12]

XX Persei has a mass of 16 solar masses, above the limit beyond which stars end their lives as supernovae.[5]

Companions

XX Persei is listed in multiple star catalogues with a companion of magnitude 9.8 223″ away.[13] This star is BD+54°445 and it is an unrelated foreground object. In addition, the spectrum of XX Persei shows absorption lines of a hot companion too close to be resolved. The combined spectral type has been given as M4Ib + B7V,[3] while the UV spectrum of the companion has been used to derive a spectral classification of A.[14]

See also

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940  Gaia DR3 record for this source at VizieR.
  2. ↑ 2.0 2.1 Kiss, L. L.; Szabó, Gy. 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. doi:10.1111/j.1365-2966.2006.10973.x. Bibcode: 2006MNRAS.372.1721K. 
  3. ↑ 3.0 3.1 Proust, D.; Ochsenbein, F.; Pettersen, B. R. (1981). "A catalogue of variable-visual binary stars". Astronomy and Astrophysics Supplement Series 44: 179. Bibcode: 1981A&AS...44..179P. 
  4. ↑ 4.0 4.1 Samus, N. N. 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. 
  5. ↑ 5.0 5.1 5.2 5.3 Stothers, R.; Leung, K. C. (1971). "Luminosities, masses and periodicities of massive red supergiants". Astronomy and Astrophysics 10: 290. Bibcode: 1971A&A....10..290S. 
  6. ↑ 6.0 6.1 6.2 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. doi:10.3847/1538-3881/ab1cbd. Bibcode: 2019AJ....158...20M. 
  7. ↑ Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
  8. ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup. 
  9. ↑ Percy, John R.; Sato, Hiromitsu (2009). "Long Secondary Periods in Pulsating Red Supergiant Stars". Journal of the Royal Astronomical Society of Canada 103 (1): 11. Bibcode: 2009JRASC.103...11P. 
  10. ↑ Reiter, Megan; Marengo, Massimo; Hora, Joseph L.; Fazio, Giovanni G. (2015). "A Spitzer/IRAC characterization of Galactic AGB and RSG stars". Monthly Notices of the Royal Astronomical Society 447 (4): 3909. doi:10.1093/mnras/stu2725. Bibcode: 2015MNRAS.447.3909R. 
  11. ↑ Fok, Thomas K. T.; Nakashima, Jun-Ichi; Yung, Bosco H. K.; Hsia, Chih-Hao; Deguchi, Shuji (2012). "Maser Observations of Westerlund 1 and Comprehensive Considerations on Maser Properties of Red Supergiants Associated with Massive Clusters". The Astrophysical Journal 760 (1): 65. doi:10.1088/0004-637X/760/1/65. Bibcode: 2012ApJ...760...65F. 
  12. ↑ Verheyen, L.; Messineo, M.; Menten, K. M. (2012). "SiO maser emission from red supergiants across the Galaxy . I. Targets in massive star clusters". Astronomy & Astrophysics 541: A36. doi:10.1051/0004-6361/201118265. Bibcode: 2012A&A...541A..36V. 
  13. ↑ Mason, B. D. et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal 122 (6): 3466, doi:10.1086/323920, Bibcode: 2001AJ....122.3466M, http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=B/wds, retrieved 2016-09-04 
  14. ↑ Buss, Richard H.; Snow, Theodore P. (1988). "Hot components and circumstellar grains in M supergiant syncretic binaries". Astrophysical Journal 335: 331. doi:10.1086/166931. Bibcode: 1988ApJ...335..331B. 



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