V424 Lacertae

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V424 Lacertae
Lacerta constellation map.svg
Red circle.svg
Location of V424 Lacertae (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Lacerta
Right ascension 22h 56m 25.99839s [1]
Declination +49° 44′ 00.7587″ [1]
Apparent magnitude  (V)+4.94 [2]
Characteristics
Spectral type K5 Ib [3]
U−B color index +1.95 [2]
B−V color index +1.77 [2]
Variable type Lc [4]
Astrometry
Radial velocity (Rv)−9.50 [5]  km/s
Proper motion (μ)RA: −0.649  mas/yr [1]
Dec.: −2.768  mas/yr [1]
Parallax (π)1.4018 ± 0.1129  mas [1]
Distance 2,300 ± 200  ly
(710 ± 60  pc)
Absolute magnitude  (MV)−4.27 [6]
Details
Mass 6.8 [7]   M☉
Radius 288+26
−21 [8]   R☉
Luminosity 16,600+4,300
−3,400 [9]   L☉
Surface gravity (log g)+0.50 [7]   cgs
Temperature 3749±49 [9]   K
Other designations
V424  Lac, BD+48° 3887, HR  8726, HD  216946, BD+48°3887, HIP  113288, SAO  52516
Database references
SIMBAD data

V424 Lacertae (V424 Lac) is a red supergiant variable star in the constellation Lacerta. It is a member of the Lacerta OB1 stellar association.

An ultraviolet band light curve light curve for V424 Lacertae, adapted from Messina (2007) V424LacLightCurve.png
An ultraviolet band light curve light curve for V424 Lacertae, adapted from Messina (2007)

The MK spectral type of V424 Lac has been determined to be K5, [3] but it has also been classified as M0. [6] It was discovered to be slightly variable using analysis of Hipparcos photometry. The total range is less than a tenth of a magnitude. [11] Multiple short periods are detected, as well as slow variations with a period of 1,100 or 1,601 days. Although listed in the General Catalogue of Variable Stars as a slow irregular variable, it has been considered to be either a semiregular variable or long secondary period variable. [10]

There is an ultraviolet excess from V424 Lacertae, that may be due to an unseen companion, which could also explain the long secondary period. On this assumption, a low-mass stellar companion in a 1,382 day 6.2 AU orbit has been suggested. [7]

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References

  1. 1 2 3 4 5 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.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  3. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373. S2CID   123149047.
  4. ↑ 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.
  5. ↑ Gontcharov, G. A. (2006). "Pulkovo Compilation of Radial Velocities for 35 495 Hipparcos stars in a common system". Astronomy Letters. 32 (11): 759–771. arXiv: 1606.08053 . Bibcode:2006AstL...32..759G. doi:10.1134/S1063773706110065. S2CID   119231169.
  6. 1 2 Levesque, Emily M.; Massey, Philip; Olsen, K. A. G.; Plez, Bertrand; Josselin, Eric; Maeder, Andre; Meynet, Georges (2005). "The Effective Temperature Scale of Galactic Red Supergiants: Cool, but Not As Cool As We Thought". The Astrophysical Journal. 628 (2): 973–985. arXiv: astro-ph/0504337 . Bibcode:2005ApJ...628..973L. doi:10.1086/430901. S2CID   15109583.
  7. 1 2 3 Lee, B.-C.; Han, I.; Park, M.-G.; Hatzes, A. P.; Kim, K.-M. (2014). "Low-amplitude and long-period radial velocity variations in giants HD 3574, 63 Cygni, and HD 216946". Astronomy & Astrophysics. 566: A124. arXiv: 1405.5955 . Bibcode:2014A&A...566A.124L. doi:10.1051/0004-6361/201321863. S2CID   54177778.
  8. ↑ Ryan Norris. "Student Science at NMT: Learning Optical Interferometry Through Projects on Evolved Stars" (PDF). CHARA.
  9. 1 2 Taniguchi, Daisuke; Matsunaga, Noriyuki; Jian, Mingjie; Kobayashi, Naoto; Fukue, Kei; Hamano, Satoshi; Ikeda, Yuji; Kawakita, Hideyo; Kondo, Sohei; Otsubo, Shogo; Sameshima, Hiroaki; Takenaka, Keiichi; Yasui, Chikako (2022-05-01). "Erratum: Effective temperatures of red supergiants estimated from line-depth ratios of iron lines in the YJ bands, 0.97-1.32 μm". Monthly Notices of the Royal Astronomical Society. 512 (2): 2669–2670. Bibcode:2022MNRAS.512.2669T. doi: 10.1093/mnras/stac686 . ISSN   0035-8711.
  10. 1 2 Messina, Sergio (2007). "Evidence for the pulsational origin of the Long Secondary Periods: The red supergiant star V424 Lac (HD 216946)". New Astronomy. 12 (7): 556–561. Bibcode:2007NewA...12..556M. doi:10.1016/j.newast.2007.04.002.
  11. ↑ Kazarovets, E. V.; Samus, N. N.; Durlevich, O. V.; Frolov, M. S.; Antipin, S. V.; Kireeva, N. N.; Pastukhova, E. N. (1999). "The 74th Special Name-list of Variable Stars". Information Bulletin on Variable Stars. 4659: 1. Bibcode:1999IBVS.4659....1K.
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