| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas [1] |
| Distance | 6,614+1,060 −812 ly (2,029+325 −249 pc) [5] |
| Absolute magnitude (MV) | −4.6 [6] |
| Details | |
| Mass | 16 [6] M☉ |
| Radius | 718+80 −56 [7] R☉ |
| Luminosity | 42,000 [8] L☉ |
| Temperature | 3,339 [5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
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.
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. [6] 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. [10]
The most likely distance of XX Per is 2,290 pc, from assumed membership of the Perseus OB1 association. [11] Gaia Data Release 3 includes a parallax of 0.3980±0.0316 mas, corresponding to a distance of around 2,500 pc. [1]
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. [12] [13]
XX Persei has a mass of 16 solar masses, above the limit beyond which stars end their lives as supernovae. [6]
XX Persei is listed in multiple star catalogues with a companion of magnitude 9.8 223 ″ away. [14] 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. [15]
- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b 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. arXiv: astro-ph/0608438. Bibcode: 2006MNRAS.372.1721K. doi: 10.1111/j.1365-2966.2006.10973.x. S2CID 5203133.
- ^ a b 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.
- ^ a b 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.
- ^ a b Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ^ a b c d Stothers, R.; Leung, K. C. (1971). "Luminosities, masses and periodicities of massive red supergiants". Astronomy and Astrophysics. 10: 290. Bibcode: 1971A&A....10..290S.
- ^ Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
- ^ 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.
- ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
- ^ 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.
- ^ 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. arXiv: 1501.02749. Bibcode: 2015MNRAS.447.3909R. doi: 10.1093/mnras/stu2725. S2CID 118515353.
- ^ 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. arXiv: 1209.6427. Bibcode: 2012ApJ...760...65F. doi: 10.1088/0004-637X/760/1/65. S2CID 53393926.
- ^ 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. arXiv: 1203.4727. Bibcode: 2012A&A...541A..36V. doi: 10.1051/0004-6361/201118265. S2CID 55630819.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920, retrieved 2016-09-04
- ^ Buss, Richard H.; Snow, Theodore P. (1988). "Hot components and circumstellar grains in M supergiant syncretic binaries". Astrophysical Journal. 335: 331. Bibcode: 1988ApJ...335..331B. doi: 10.1086/166931.
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| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| 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 mas [1] |
| Distance | 6,614+1,060 −812 ly (2,029+325 −249 pc) [5] |
| Absolute magnitude (MV) | −4.6 [6] |
| Details | |
| Mass | 16 [6] M☉ |
| Radius | 718+80 −56 [7] R☉ |
| Luminosity | 42,000 [8] L☉ |
| Temperature | 3,339 [5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
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.
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. [6] 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. [10]
The most likely distance of XX Per is 2,290 pc, from assumed membership of the Perseus OB1 association. [11] Gaia Data Release 3 includes a parallax of 0.3980±0.0316 mas, corresponding to a distance of around 2,500 pc. [1]
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. [12] [13]
XX Persei has a mass of 16 solar masses, above the limit beyond which stars end their lives as supernovae. [6]
XX Persei is listed in multiple star catalogues with a companion of magnitude 9.8 223 ″ away. [14] 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. [15]
- ^ a b c d e f Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211. Bibcode: 2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
- ^ a b 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. arXiv: astro-ph/0608438. Bibcode: 2006MNRAS.372.1721K. doi: 10.1111/j.1365-2966.2006.10973.x. S2CID 5203133.
- ^ a b 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.
- ^ a b 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.
- ^ a b Norris, Ryan P. (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (PDF) (PhD). Georgia State University.
- ^ a b c d Stothers, R.; Leung, K. C. (1971). "Luminosities, masses and periodicities of massive red supergiants". Astronomy and Astrophysics. 10: 290. Bibcode: 1971A&A....10..290S.
- ^ Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
- ^ 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.
- ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 6 January 2022.
- ^ 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.
- ^ 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. arXiv: 1501.02749. Bibcode: 2015MNRAS.447.3909R. doi: 10.1093/mnras/stu2725. S2CID 118515353.
- ^ 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. arXiv: 1209.6427. Bibcode: 2012ApJ...760...65F. doi: 10.1088/0004-637X/760/1/65. S2CID 53393926.
- ^ 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. arXiv: 1203.4727. Bibcode: 2012A&A...541A..36V. doi: 10.1051/0004-6361/201118265. S2CID 55630819.
- ^ Mason, B. D.; et al. (2014), "The Washington Visual Double Star Catalog", The Astronomical Journal, 122 (6): 3466, Bibcode: 2001AJ....122.3466M, doi: 10.1086/323920, retrieved 2016-09-04
- ^ Buss, Richard H.; Snow, Theodore P. (1988). "Hot components and circumstellar grains in M supergiant syncretic binaries". Astrophysical Journal. 335: 331. Bibcode: 1988ApJ...335..331B. doi: 10.1086/166931.
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Star clusters |
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| Nebulae |
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| Galaxies |
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