Astronomy:HR 3831
Coordinates: 
09h 36m 25.4069s, −48° 45′ 04.2549″
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Vela |
| Right ascension | 09h 36m 25.4069s[1] |
| Declination | –48° 45′ 04.2549″[1] |
| Apparent magnitude (V) | 6.232 |
| Characteristics | |
| HD 83368A | |
| Spectral type | A8V[1] |
| Apparent magnitude (G) | 6.219[2] |
| Variable type | Rapidly oscillating Ap |
| HD 83368B | |
| Spectral type | F9V[3] |
| Apparent magnitude (G) | 8.995[4] |
| Astrometry | |
| HD 83368A | |
| Proper motion (μ) | RA: -8.16±0.03[2] mas/yr Dec.: -18.85±0.03[2] mas/yr |
| Parallax (π) | 14.01 ± 0.03[2] mas |
| Distance | 232.8 ± 0.5 ly (71.4 ± 0.2 pc) |
| HD 83368B | |
| Radial velocity (Rv) | -4.0±0.3[4] km/s |
| Proper motion (μ) | RA: -9.41±0.19 mas/yr Dec.: -14.00±0.17 mas/yr |
| Parallax (π) | 14.31 ± 0.15[4] mas |
| Distance | 228 ± 2 ly (69.9 ± 0.7 pc) |
| Details | |
| HD 83368A | |
| Mass | 1.78+0.12−0.17[5] M☉ |
| Radius | 2.003[6] R☉ |
| Luminosity (bolometric) | 12.33[6] L☉ |
| Surface gravity (log g) | 4.2[6] cgs |
| Temperature | 7650[6] K |
| Rotation | 2.851976±0.00003 d[6] |
| Rotational velocity (v sin i) | 33.8±1.0[5] km/s |
| Age | 0.93+0.42−0.34[5] Gyr |
| HD 83368B | |
| Surface gravity (log g) | 4 cgs |
| Other designations | |
| HD 83368A: 2MASS J09362541-4845042, TYC 8176-283-1 | |
| HD 83368B: 2MASS J09362537-4845072, Gaia DR2 5410092611662456704, TYC 8176-2818-1 | |
| Database references | |
| SIMBAD | data |
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.[4]
The star system is a visual binary with a 3.29″ projected separation,[6] identified as such in 2002.[7] 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.[8] The primary star is chemically peculiar, exhibiting spots of enhanced concentrations of lithium, europium and oxygen.[6]
See also
- Vela (Chinese astronomy)
References
- ↑ 1.0 1.1 1.2 1.3 "HD 83368". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+83368.
- ↑ 2.0 2.1 2.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ "HD 83368B". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=HD+83368B.
- ↑ 4.0 4.1 4.2 4.3 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 5.0 5.1 5.2 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, doi:10.1093/mnras/sty3105, Bibcode: 2019MNRAS.483.2300S
- ↑ 6.0 6.1 6.2 6.3 6.4 6.5 6.6 Kochukhov, O. (2005), "Pulsational line profile variation of the roAp star HR 3831", Astronomy & Astrophysics 446 (3): 1051–1070, doi:10.1051/0004-6361:20053345
- ↑ Schöller, M.; Correia, S.; Hubrig, S.; Kurtz, D. W. (2002), "Multiplicity of rapidly oscillating Ap stars", Astronomy & Astrophysics 545: A38, doi:10.1051/0004-6361/201118538
- ↑ Bigot, L.; Kurtz, D. W. (2011), "Theoretical light curves of dipole oscillations in roAp stars", Astronomy & Astrophysics 536: A73, doi:10.1051/0004-6361/201116981, Bibcode: 2011A&A...536A..73B
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