SU Persei

SU Persei
Location of SU Persei (circled) near the Double Cluster (north is towards bottom right)
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Perseus[1]
Right ascension 02h 22m 06.89s[2]
Declination +56° 36′ 14.9″[2]
Apparent magnitude (V) 7.2 - 8.7[3]
Characteristics
Evolutionary stage red supergiant[4]
Spectral type M3.5Iab[3]
Variable type SRc[3]
Astrometry
Radial velocity (Rv)−44.8±0.3[4] km/s
Proper motion (μ) RA: −0.765[2] mas/yr
Dec.: −1.204[2] mas/yr
Parallax (π)0.4168±0.0279 mas[2]
Distance7,800 ± 500 ly
(2,400 ± 200 pc)
Absolute magnitude (MV)−5.78[5]
Details
Mass13±4[6] M☉
Radius1,044+31
−21 – 1,139+34
−23[6] R☉
Luminosity91,201[5] L☉
Surface gravity (log g)−0.1[7] cgs
Temperature3,650±50[6] K
Other designations
SU Persei, BD+55°597, HD 14469,[8]
ASASSN-V J022206.86+563614.8[3]
Database references
SIMBADdata

SU Persei is a red supergiant star located in the constellation of Perseus. It is located within the Double Cluster, 7,250+470
−420 light-years away.[10] It is a semiregular variable star[3] that ranges in brightness from magnitude 7.2 to 8.7,[3] which makes it too faint to be seen with the naked eye, but can be seen with binoculars or a telescope.

SU Persei was imaged by the CHARA array in 2015, 2016, 2019, 2020, and 2021.[11] Observations during 2015 and 2016 with CHARA show that the star has an angular diameter between 3.51 and 3.68 milliarcseconds. Considering its large distance from Earth, this results in a radius between 1,044 and 1,139 times that of the Sun, making it one of the largest stars known.[6]

SU Persei is losing mass at a rate of 1.62+0.72
−0.63×10−6 M☉ per year, via a stellar wind.[12]

In 1907, Henrietta Swan Leavitt discovered that the star's brightness varies by examining photographic plates.[13] It was given its variable star designation, SU Persei, in 1908.[14]

See also

References

  1. ^ Anderson, E.; Francis, Ch. (May 2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331–346. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. eISSN 1562-6873. ISSN 1063-7737. S2CID 119257644.
  2. ^ a b c d e 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.
  3. ^ a b c d e f "SU Per". International Variable Star Index. Retrieved 2025-03-30.
  4. ^ a b De Burgos, A.; Simon-Díaz, S.; Lennon, D. J.; Dorda, R.; Negueruela, I.; Urbaneja, M. A.; Patrick, L. R.; Herrero, A. (2020). "High-resolution spectroscopic study of massive blue and red supergiants in Perseus OB1. I. Definition of the sample, membership, and kinematics". Astronomy and Astrophysics. 643: A116. arXiv:2008.13299. Bibcode:2020A&A...643A.116D. doi:10.1051/0004-6361/202039019.
  5. ^ a b Massey, Philip; Silva, David R.; Levesque, Emily M.; Plez, Bertrand; Olsen, Knut A. G.; Clayton, Geoffrey C.; Meynet, Georges; Maeder, Andre (2009). "Red Supergiants in the Andromeda Galaxy (M31)". The Astrophysical Journal. 703 (1): 420. arXiv:0907.3767. Bibcode:2009ApJ...703..420M. doi:10.1088/0004-637X/703/1/420.
  6. ^ a b c d Norris, Ryan (2019). Seeing Stars Like Never Before: A Long-term Interferometric Imaging Survey of Red Supergiants (Thesis). Georgia State University. doi:10.57709/15009706.
  7. ^ Dicenzo, Brooke; Levesque, Emily M. (2019). "Atomic Absorption Line Diagnostics for the Physical Properties of Red Supergiants". The Astronomical Journal. 157 (4): 167. arXiv:1902.01862. Bibcode:2019AJ....157..167D. doi:10.3847/1538-3881/ab01cb.
  8. ^ "SU Persei". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 2025-03-30.
  9. ^ "ASAS-SN Variable Stars Database". ASAS-SN Variable Stars Database. ASAS-SN. Retrieved 30 March 2025.
  10. ^ Bailer-Jones, C. A. L.; Rybizki, J.; Fouesneau, M.; Demleitner, M.; Andrae, R. (February 2021). "Estimating Distances from Parallaxes. V. Geometric and Photogeometric Distances to 1.47 Billion Stars in Gaia Early Data Release 3". The Astronomical Journal. 161 (3): 147. arXiv:2012.05220. Bibcode:2021AJ....161..147B. doi:10.3847/1538-3881/abd806. ISSN 1538-3881.
  11. ^ Norris, Ryan (2023). "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
  12. ^ Decin, L.; Richards, A. M. S.; Marchant, P.; Sana, H. (January 2024). "ALMA detection of CO rotational line emission in red supergiant stars of the massive young star cluster RSGC1. Determination of a new mass-loss rate prescription for red supergiants" (PDF). Astronomy & Astrophysics. 681: A17. Bibcode:2024A&A...681A..17D. doi:10.1051/0004-6361/202244635. Retrieved 31 March 2025.
  13. ^ Leavitt, Henrietta S.; Pickering, Edward C. (April 1907). "New Variable Stars in Harvard Map, Nos. 3 and 6". Harvard College Observatory Circular. 127: 1–4. Bibcode:1907HarCi.127....1L. Retrieved 30 March 2025.
  14. ^ Dunér, Nils Christofer; Hartwig, Ernst; Müller, G. (October 1908). "Benennung von neu entdeckten veränderlichen Sternen". Astronomische Nachrichten. 179 (6): 85. Bibcode:1908AN....179...85D. doi:10.1002/asna.19081790602. Retrieved 30 March 2025.


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