Astronomy:PR Persei
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Short description: Red Supergiant star in the constellation Perseus
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| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Perseus |
| Right ascension | 02h 21m 42.41s[1] |
| Declination | +57° 51′ 46.1″[1] |
| Apparent magnitude (V) | 7.7 – 8.2[2] |
| Characteristics | |
| Evolutionary stage | Red supergiant |
| Spectral type | M1 Iab-Ib[2] |
| Variable type | LC[2] |
| Astrometry | |
| Radial velocity (Rv) | −45.9[1] km/s |
| Proper motion (μ) | RA: −0.857[1] mas/yr Dec.: −1.059[1] mas/yr |
| Parallax (π) | 0.3621 ± 0.0239[1] mas |
| Distance | 9,000 ± 600 ly (2,800 ± 200 pc) |
| Details | |
| Mass | 9.2[3] M☉ |
| Radius | 401[4] R☉ |
| Luminosity | 27,542[5] L☉ |
| Surface gravity (log g) | 0.89[6] cgs |
| Temperature | 3,715[5] K |
| Metallicity [Fe/H] | −0.22[6] dex |
| Other designations | |
| Database references | |
| SIMBAD | data |
PR Persei (also known as HD 14404, HIP 10995, or BD+57 550) is a red supergiant star located in the constellation of Perseus in the northern celestial hemisphere. Classified as a variable star of spectral type M1-Iab-Ib, it exhibits mild brightness variations due to pulsations in its outer layers. It resides in the Milky Way galaxy, approximately 9,000 light-years from the Solar System. It can be seen near the Double Cluster of Perseus through a telescope or binoculars.
Charecterstics
PR Persei is a cool, luminous red supergiant with a spectral type of M1 Iab-Ib, indicating an intermediate luminosity class between Iab and Ib supergiants.[9]
References
- ↑ 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.
- ↑ 2.0 2.1 2.2 "PR Persei". AAVSO. https://vsx.aavso.org/index.php?view=detail.top&oid=25840.
- ↑ Anders, F.; Khalatyan, A.; Queiroz, A. B. A.; Chiappini, C.; Ardèvol, J.; Casamiquela, L.; Figueras, F.; Jiménez-Arranz, Ó. et al. (2022). "Photo-astrometric distances, extinctions, and astrophysical parameters for Gaia EDR3 stars brighter than G = 18.5". Astronomy and Astrophysics 658: A91. doi:10.1051/0004-6361/202142369. Bibcode: 2022A&A...658A..91A.
- ↑ Fetherolf, Tara; Pepper, Joshua; Simpson, Emilie; Kane, Stephen R.; Močnik, Teo; English, John Edward; Antoci, Victoria; Huber, Daniel et al. (2023). "Variability Catalog of Stars Observed during the TESS Prime Mission". The Astrophysical Journal Supplement Series 268 (1): 4. doi:10.3847/1538-4365/acdee5. Bibcode: 2023ApJS..268....4F.
- ↑ 5.0 5.1 Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020). "Short-term Variability of Evolved Massive Stars with TESS. II. A New Class of Cool, Pulsating Supergiants". The Astrophysical Journal 902 (1): 24. doi:10.3847/1538-4357/abb318. Bibcode: 2020ApJ...902...24D.
- ↑ 6.0 6.1 Huson, Dylan; Cowan, Indiana; Sizemore, Logan; Kounkel, Marina; Hutchinson, Brian (2025). "Gaia Net: Toward Robust Spectroscopic Parameters of Stars of all Evolutionary Stages". The Astrophysical Journal 984 (1): 58. doi:10.3847/1538-4357/adc2fa. Bibcode: 2025ApJ...984...58H.
- ↑ "PR Persei". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=PR+Persei.
- ↑ EAS (1997). "The HIPPARCOS and TYCHO catalogues". Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series (Noordwijk, Netherlands: ESA Publications Division) 1200. ISBN 9290923997. Bibcode: 1997HIP...C......0E. https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats. Retrieved 26 October 2025.
- ↑ Dorn-Wallenstein, Trevor Z.; Levesque, Emily M.; Neugent, Kathryn F.; Davenport, James R. A.; Morris, Brett M.; Gootkin, Keyan (2020-10-01). "Short-term Variability of Evolved Massive Stars with TESS. II. A New Class of Cool, Pulsating Supergiants". The Astrophysical Journal 902 (1): 24. doi:10.3847/1538-4357/abb318. ISSN 0004-637X. Bibcode: 2020ApJ...902...24D.
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