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HD 3346

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HD 3346

A light curve for V428 Andromedae, plotted from TESS data,[1]
Observation data
Epoch J2000      Equinox J2000
Constellation Andromeda
Right ascension 00h 36m 46.44107s[2]
Declination +44° 29′ 18.9202″[2]
Apparent magnitude (V) 5.13 – 5.19[3]
Characteristics
Spectral type K6 IIIa[4] (K5 - M0 III[3])
B−V color index 1.587±0.005[5]
Variable type SRS[3]
Astrometry
Radial velocity (Rv)−33.46±0.22[2] km/s
Proper motion (μ) RA: −37.121 mas/yr[2]
Dec.: +32.293 mas/yr[2]
Parallax (π)4.7240 ± 0.0894 mas[2]
Distance690 ± 10 ly
(212 ± 4 pc)
Absolute magnitude (MV)−1.23[5]
Orbit[6]
Period (P)576.2±3.5 d
Eccentricity (e)0.30±0.06
Periastron epoch (T)43787±22 MJD
Argument of periastron (ω)
(secondary)		279±15°
Semi-amplitude (K1)
(primary)		0.69±0.08 km/s
Details
Radius69.98±2.98[7] R☉
Luminosity979.2±76.65[7] L☉
Surface gravity (log g)1.19±0.16[8] cgs
Temperature3909±170[8] K
Metallicity [Fe/H]−0.00±0.10[8] dex
Other designations
V428 Andromedae, BD+43°113, HD 3346, HIP 2900, HR 152, SAO 36509, PPM 43119[9]
Database references
SIMBADdata

HD 3346, also known as V428 Andromedae, is a binary star[10] system in the northern constellation of Andromeda. It is a dim star but visible to the naked eye under suitable viewing conditions, having an apparent visual magnitude of 5.14.[5] The distance to HD 3346 can be determined from its annual parallax shift of 4.72 mas.[2] This yields a range of about 690 light-years (210 parsecs). At that distance the brightness of the system is diminished by an extinction of 0.16 magnitude due to interstellar dust.[11] It is moving closer to the Earth with a heliocentric radial velocity of −33 km/s.[11]

Binary system

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This is a single-lined spectroscopic binary system with an orbital period of 576 days and an eccentricity of 0.3. The a sin i value for the primary is 5.1 ± 0.6 Gm (0.0341 ± 0.0040 AU), where a is the semimajor axis and i is the (unknown) orbital inclination. The provides a minimum value for the actual semimajor axis.[6]

The visible component is a red giant star and has been defined as a standard star for the stellar classification of K6 IIIa.[4] Prior to that there had been no spectral standard for K6 giants and HD 3346 had been classified between K5 III and M0 III.[12]

In 1996 it was announced that the variations in radial velocity of this star were larger than expected. Two orbiting companions were proposed to explain this variation, the one known since 1985 with a period of about 650 days and a minimum mass of about 60 MJ, and a second one with a period of about 14-40 days and a minimum mass of about 10 MJ.[13][14] The existence of this second, possibly planetary companion was never confirmed.

Variability

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In 1982, HD 3346 was listed as a suspected variable star (NSV 15135) in Pavel Nikolaevich Kholopov's catalog of suspected variable stars.[15] Gregory W. Henry et al. confirmed that the star is variable in year 2000.[16] It was given its variable star designation, V428 Andromedae, in 2003.[17]

It is a short-period semi-regular variable (type SRS),[3] also called an ultra-small-amplitude pulsating red giant.[18] It has an amplitude of only 0.065 magnitudes.[18] The main pulsation period is 11.5 days, but other periods of 11, 15, and 22 days have been detected.[19][18]

References

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  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 26 August 2024.
  2. ^ 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.
  3. ^ a b c d N. N. Samus; O. V. Durlevich; et al. "V428 And database entry". Combined General Catalog of Variable Stars (2017 ed.). CDS. Retrieved 2018-11-12.
  4. ^ a b 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.
  5. ^ a b c Anderson, E.; Francis, Ch. (2012). "XHIP: An extended hipparcos compilation". Astronomy Letters. 38 (5): 331. arXiv:1108.4971. Bibcode:2012AstL...38..331A. doi:10.1134/S1063773712050015. S2CID 119257644.
  6. ^ a b McClure, R. D.; et al. (August 1985), "A spectroscopic orbit for HR 152", Publications of the Astronomical Society of the Pacific, 97: 740–744, Bibcode:1985PASP...97..740M, doi:10.1086/131600, S2CID 121308350
  7. ^ a b van Belle, Gerard T.; von Braun, Kaspar; Ciardi, David R.; Pilyavsky, Genady; Buckingham, Ryan S.; Boden, Andrew F.; Clark, Catherine A.; Hartman, Zachary; van Belle, Gerald; Bucknew, William; Cole, Gary (2021-12-01). "Direct Measurements of Giant Star Effective Temperatures and Linear Radii: Calibration against Spectral Types and V - K Color". The Astrophysical Journal. 922 (2): 163. arXiv:2107.09205. Bibcode:2021ApJ...922..163V. doi:10.3847/1538-4357/ac1687. ISSN 0004-637X. V428 Andromedae's database entry at VizieR.
  8. ^ a b c Röck, B.; Vazdekis, A.; Peletier, R. F.; Knapen, J. H.; Falcón-Barroso, J. (2015). "Stellar population synthesis models between 2.5 and 5 μm based on the empirical IRTF stellar library". Monthly Notices of the Royal Astronomical Society. 449 (3): 2853–2874. arXiv:1505.01837. Bibcode:2015MNRAS.449.2853R. doi:10.1093/mnras/stv503.
  9. ^ "HD 3167". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved October 6, 2018.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  11. ^ a b Famaey, B.; et al. (January 2005). "Local kinematics of K and M giants from CORAVEL/Hipparcos/Tycho-2 data. Revisiting the concept of superclusters". Astronomy and Astrophysics. 430 (1): 165–186. arXiv:astro-ph/0409579. Bibcode:2005A&A...430..165F. doi:10.1051/0004-6361:20041272. S2CID 17804304.
  12. ^ Keenan, P. C.; Pitts, R. E. (1980). "Revised MK spectral types for G, K ANS M stars". The Astrophysical Journal Supplement Series. 42: 541. Bibcode:1980ApJS...42..541K. doi:10.1086/190662.
  13. ^ Noyes, R.; et al. (1996). "HD 3346". IAU Circular. 6316 (6316): 1. Bibcode:1996IAUC.6316....1N.
  14. ^ Bell, George H. (2001-04-05). "The Search for the Extrasolar Planets: A Brief History of the Search, the Findings and the Future Implications". Arizona State University. Retrieved 2008-07-16.
  15. ^ Kholopov, P. N. (1982). New catalogue of stars suspected of variability containing data on 14810 variable stars which have not received definite nomenclature until 1980. Moskva: Nauka. p. 359. Bibcode:1982ncss.book.....K.
  16. ^ Henry, Gregory W.; Fekel, Francis C.; Henry, Stephen M.; Hall, Douglas S. (September 2000). "Photometric Variability in a Sample of 187 G and K Giants". The Astrophysical Journal Supplement Series. 130 (1): 201–225. Bibcode:2000ApJS..130..201H. doi:10.1086/317346. Retrieved 6 November 2024.
  17. ^ Kazarovets, E. V.; Kireeva, N. N.; Samus, N. N.; Durlevich, O. V. (May 2003). "The 77th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 5422. Bibcode:2003IBVS.5422....1K. Retrieved 6 November 2024.
  18. ^ a b c Percy, John R.; et al. (December 2001), "Periods of Eleven K5-M0 Pulsating Red Giants", Information Bulletin on Variable Stars, 5209: 1, Bibcode:2001IBVS.5209....1P
  19. ^ Glass, I. S.; Van Leeuwen, F. (2007). "Semiregular variables in the solar neighbourhood". Monthly Notices of the Royal Astronomical Society. 378 (4): 1543–1549. arXiv:0704.3150. Bibcode:2007MNRAS.378.1543G. doi:10.1111/j.1365-2966.2007.11903.x. S2CID 14332208.
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