HR 3831

HR 3831

A light curve for IM Velorum (HR 3831), plotted from TESS data.[1] The 2.852 day period[2] is shown in red.
Observation data
Epoch J2000      Equinox J2000
Constellation Vela
Right ascension 09h 36m 25.4069s[3]
Declination –48° 45′ 04.2549″[3]
Apparent magnitude (V) 6.232
Characteristics
HD 83368A
Spectral type A8V[3]
Apparent magnitude (G) 6.219[4]
Variable type Rapidly oscillating Ap
HD 83368B
Spectral type F9V[5]
Apparent magnitude (G) 8.995[6]
Astrometry
HD 83368A
Proper motion (μ) RA: -8.16±0.03 mas/yr[4]
Dec.: -18.85±0.03 mas/yr[4]
Parallax (π)14.01 ± 0.03 mas[4]
Distance232.8 ± 0.5 ly
(71.4 ± 0.2 pc)
HD 83368B
Radial velocity (Rv)-4.0±0.3[6] km/s
Proper motion (μ) RA: -9.41±0.19 mas/yr[6]
Dec.: -14.00±0.17 mas/yr[6]
Parallax (π)14.31 ± 0.15 mas[6]
Distance228 ± 2 ly
(69.9 ± 0.7 pc)
Details
HD 83368A
Mass1.78+0.12
−0.17[7] M☉
Radius2.003[8] R☉
Luminosity (bolometric)12.33[8] L☉
Surface gravity (log g)4.2[8] cgs
Temperature7650[8] K
Rotation2.851976±0.00003 d[8]
Rotational velocity (v sin i)33.8±1.0[7] km/s
Age0.93+0.42
−0.34[7] Gyr
HD 83368B
Surface gravity (log g)4 cgs
Other designations
CD−48 4831, HD 83368, HIP 47145, HR 3831, SAO 221339, GSC 08176-00283, IM Vel[3]
HD 83368A: 2MASS J09362541-4845042, TYC 8176-283-1
HD 83368B: 2MASS J09362537-4845072, Gaia DR2 5410092611662456704, TYC 8176-2818-1
Database references
SIMBADdata

HR 3831, also known as HD 83368, is a binary star system in the southern constellation of Vela at a distance of 233 light years. This object is barely visible to the naked eye as a dim, blue star with an apparent visual magnitude of 6.232. It is approaching the Earth with a heliocentric radial velocity of 4.0±0.3 km/s.[6]

The star system is a visual binary with a 3.29″ projected separation,[8] identified as such in 2002.[9] The larger star, HD 83368A, is a pulsating variable of a rapidly oscillating Ap type. It has a single yet strongly distorted dipole pulsation mode with a frequency of 1427 μHz.[10] The primary star is chemically peculiar, exhibiting spots of enhanced concentrations of lithium, europium and oxygen.[8]

The star's variability was discovered by Pierre Renson, and announced in 1977.[11] It was given its variable star designation, IM Velorum, in 1981.[12]

See also

References

  1. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 27 September 2024.
  2. ^ Kurtz, D. W.; van Wyk, F; Roberts, G.; Marang, F.; Handler, G.; Medupe, R.; Kilkenny, D. (May 1997). "Frequency variability in the rapidly oscillating AP star HR 3831: three more years of monitoring". Monthly Notices of the Royal Astronomical Society. 287 (1): 69–78. Bibcode:1997MNRAS.287...69K. doi:10.1093/mnras/287.1.69.
  3. ^ a b c d "HD 83368". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved June 30, 2021.
  4. ^ a b c Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  5. ^ "HD 83368B". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved June 30, 2021.
  6. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  7. ^ a b c Sikora, J.; Wade, G. A.; Power, J.; Neiner, C. (2019), "A volume-limited survey of MCP stars within 100 pc – I. Fundamental parameters and chemical abundances", Monthly Notices of the Royal Astronomical Society, 483 (2): 2300–2324, arXiv:1811.05633, Bibcode:2019MNRAS.483.2300S, doi:10.1093/mnras/sty3105
  8. ^ a b c d e f g Kochukhov, O. (2005), "Pulsational line profile variation of the roAp star HR 3831", Astronomy & Astrophysics, 446 (3): 1051–1070, arXiv:astro-ph/0509446, doi:10.1051/0004-6361:20053345, S2CID 13102520
  9. ^ Schöller, M.; Correia, S.; Hubrig, S.; Kurtz, D. W. (2002), "Multiplicity of rapidly oscillating Ap stars", Astronomy & Astrophysics, 545: A38, arXiv:1208.0480, doi:10.1051/0004-6361/201118538, S2CID 119311263
  10. ^ Bigot, L.; Kurtz, D. W. (2011), "Theoretical light curves of dipole oscillations in roAp stars", Astronomy & Astrophysics, 536: A73, arXiv:1110.0988, Bibcode:2011A&A...536A..73B, doi:10.1051/0004-6361/201116981, S2CID 54532822
  11. ^ Renson, P. (20 May 1977). "Periodicite d'Etoiles Ap Australes" (PDF). Invormal Bulletin on Variable Stars. 1280: 1. Bibcode:1977IBVS.1280....1R. Retrieved 20 October 2024.
  12. ^ Kholopov, P. N.; Samus, N. N.; Kukarkina, N. P.; Medvedeva, G. I.; Perova, N. B. (February 1981). "65th Name-List of Variable Stars" (PDF). Information Bulletin on Variable Stars. 1921: 1. Bibcode:1981IBVS.1921....1K. Retrieved 20 October 2024.