Astronomy:SU Persei

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Short description: Star in the constellation Perseus
SU Persei
Location of SU Persei (circled) near the Double Cluster (north is towards bottom right)
Observation data
Equinox J2000.0]] (ICRS)
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[2] mas
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
A light curve for SU Persei, plotted from ASAS-SN data[9]

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. doi:10.1134/S1063773712050015. ISSN 1063-7737. Bibcode: 2012AstL...38..331A. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 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.
  3. ↑ 3.0 3.1 3.2 3.3 3.4 3.5 "SU Per". https://www.aavso.org/vsx/index.php?view=detail.top&oid=25545. 
  4. ↑ 4.0 4.1 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. doi:10.1051/0004-6361/202039019. Bibcode: 2020A&A...643A.116D. 
  5. ↑ 5.0 5.1 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. doi:10.1088/0004-637X/703/1/420. Bibcode: 2009ApJ...703..420M. 
  6. ↑ 6.0 6.1 6.2 6.3 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 Check |doi= value (help).
  7. ↑ Dicenzo, Brooke; Levesque, Emily M. (2019). "Atomic Absorption Line Diagnostics for the Physical Properties of Red Supergiants". The Astronomical Journal 157 (4): 167. doi:10.3847/1538-3881/ab01cb. Bibcode: 2019AJ....157..167D. 
  8. ↑ "SU Persei". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=SU+Persei. 
  9. ↑ "ASAS-SN Variable Stars Database". ASAS-SN. https://asas-sn.osu.edu/variables/lookup. 
  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" (in en). The Astronomical Journal 161 (3): 147. doi:10.3847/1538-3881/abd806. ISSN 1538-3881. Bibcode: 2021AJ....161..147B. 
  11. ↑ Norris, Ryan (2023). "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars". CHARA. https://www.chara.gsu.edu/files/2023Meeting/Norris_NMT_Students_2023.pdf. 
  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". Astronomy & Astrophysics 681: A17. doi:10.1051/0004-6361/202244635. Bibcode: 2024A&A...681A..17D. https://www.aanda.org/articles/aa/pdf/2024/01/aa44635-22.pdf. 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. https://articles.adsabs.harvard.edu/pdf/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. doi:10.1002/asna.19081790602. Bibcode: 1908AN....179...85D. https://articles.adsabs.harvard.edu/pdf/1909AN....179...85D. Retrieved 30 March 2025. 



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