Astronomy:V2052 Ophiuchi
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ophiuchus |
| Right ascension | 17h 56m 18.40012s[2] |
| Declination | +00° 40′ 13.2733″[2] |
| Apparent magnitude (V) | 5.81 – 5.84[3] |
| Characteristics | |
| Spectral type | B2 IV–V[4] |
| U−B color index | −0.66[5] |
| B−V color index | +0.09[5] |
| Variable type | β Cephei[3] |
| Astrometry | |
| Proper motion (μ) | RA: −4.997±0.038[2] mas/yr Dec.: −0.369±0.038[2] mas/yr |
| Parallax (π) | 3.5446 ± 0.0453[2] mas |
| Distance | 920 ± 10 ly (282 ± 4 pc) |
| Absolute magnitude (MV) | −2.54[6] |
| Details | |
| Mass | 8.9±0.7[7] M☉ |
| Radius | 4.1±0.2[8] R☉ |
| Luminosity | 3,426[2] L☉ |
| Surface gravity (log g) | 4.00[4] cgs |
| Temperature | 23,000±1,000[4] K |
| Metallicity [Fe/H] | +0.012[2] dex |
| Rotation | 3.638833±0.000003 d[9] |
| Rotational velocity (v sin i) | 60[9] km/s |
| Age | 21[10] Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
V2052 Ophiuchi, also known as HR 6684, is a star about 920 light years from Earth in the constellation Ophiuchus.[2] It is a 5th-magnitude star, making it faintly visible to the naked eye of an observer far from city lights. V2052 Ophiuchi is a Beta Cephei variable (β Cep) star, varying slightly in brightness from magnitude 5.81 to 5.84 over a period of about 3.4 hours.[3]
In 1972, Mikolaj Jerzykiewicz announced that HR 6684 is a variable star, based on his observations using the 0.6 meter Air Force Telescope on Mauna Kea. He classified the star as a β Cep variable with period of 0.13989 days, He further noted that if confirmed, it would be the least luminous and shortest period β Cep star known up to that date.[12] Spectroscopic and photometric observations by D. Harold McNamara and Bruce Bills in 1973 confirmed Jerzykiewicz's results.[13] In 1973, HR 6684 was given the variable star designation V2052 Ophiuchi.[14]
In 1994, Henryk Cugier et al. determined that V2052 Ophiuchi pulsated primarily in the fundamental (l=0) radial mode.[15] A much less powerful non-radial pulsation mode was identified in 2003.[8] Ultraviolet observations by the TD-1A satellite show that throughout its pulsation cycle, the temperature of V2052 Ophiuchi varies by 1040±880 K, and its radius changes by 3.1%±0.9%.[5] Observations at the Pic du Midi Observatory showed that V2052 Ophiuchi has a dipole magnetic field, the axis of which is offset from the star's center, and there are helium spots on the surface near the magnetic poles.[9] V2052 Ophiuchi is a type of chemically peculiar star known as a helium-strong star. Its surface is over-abundant in helium, and under-abundant in oxygen, perhaps due to its magnetic field differentially effecting the diffusion of elements in its atmosphere.[8]
References
- ↑ EAS (1997). "The HIPPARCOS and TYCHO catalogues". Astrometric and Photometric Star Catalogues Derived from the ESA Hipparcos Space Astrometry Mission. ESA SP Series (Noordwijk, Netherlands: ESA Publications Division) 1200. ISBN 9290923997. Bibcode: 1997ESASP1200.....E. https://cdsarc.cds.unistra.fr/viz-bin/ftp-index?/ftp/cats/more/HIP/cdroms/cats. Retrieved 15 October 2022.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 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.
- ↑ 3.0 3.1 3.2 Samus', N. N.; Kazarovets, E. V.; Durlevich, O. V.; Kireeva, N. N.; Pastukhova, E. N. (2017). "General catalogue of variable stars: Version GCVS 5.1". Astronomy Reports 61 (1): 80. doi:10.1134/S1063772917010085. Bibcode: 2017ARep...61...80S.
- ↑ 4.0 4.1 4.2 Morel, T.; Butler, K.; Aerts, C.; Neiner, C.; Briquet, M. (October 2006). "Abundance analysis of prime B-type targets for asteroseismology. I. Nitrogen excess in slowly-rotating β Cephei stars". Astronomy and Astrophysics 457 (2): 651–663. doi:10.1051/0004-6361:20065171. Bibcode: 2006A&A...457..651M.
- ↑ 5.0 5.1 5.2 Beeckmans, F.; Burger, M. (December 1977). "Ultraviolet observations of beta Canis Majoris stars with the TD-1 A satellite". Astronomy and Astrophysics 61: 815–826. Bibcode: 1977A&A....61..815B.
- ↑ Melnik, A. M.; Dambis, A. K. (2020). "Distance scale for high-luminosity stars in OB associations and in field with Gaia DR2. Spurious systematic motions". Astrophysics and Space Science 365 (7): 112. doi:10.1007/s10509-020-03827-0. Bibcode: 2020Ap&SS.365..112M.
- ↑ Briquet, M.; Neiner, C.; Aerts, C.; Morel, T.; Mathis, S.; Reese, D. R.; Lehmann, H.; Costero, R. et al. (November 2012). "Multisite spectroscopic seismic study of the β Cep star V2052 Ophiuchi: inhibition of mixing by its magnetic field". Monthly Notices of the Royal Astronomical Society 427 (1): 483–493. doi:10.1111/j.1365-2966.2012.21933.x. Bibcode: 2012MNRAS.427..483B.
- ↑ 8.0 8.1 8.2 Neiner, C.; Henrichs, H. F.; Floquet, M.; Frémat, Y.; Preuss, O.; Hubert, A. M.; Geers, V. C.; Tijani, A. H. et al. (December 2003). "Rotation, pulsations and magnetic field in V 2052 Ophiuchi: A new He-strong star". Astronomy and Astrophysics 411 (3): 565–579. doi:10.1051/0004-6361:20031342. Bibcode: 2003A&A...411..565N.
- ↑ 9.0 9.1 9.2 Neiner, C.; Alecian, E.; Briquet, M.; Floquet, M.; Frémat, Y.; Martayan, C.; Thizy, O.; MiMeS Collaboration (January 2012). "Detecting and modelling the magnetic field of the β Cephei star V 2052 Ophiuchi". Astronomy and Astrophysics 537: A148. doi:10.1051/0004-6361/201117941. Bibcode: 2012A&A...537A.148N.
- ↑ Tetzlaff, N.; Neuhäuser, R.; Hohle, M. M. (October 12, 2010). "A catalogue of young runaway Hipparcos stars within 3 kpc from the Sun". Monthly Notices of the Royal Astronomical Society (Oxford University Press (OUP)) 410 (1): 190–200. doi:10.1111/j.1365-2966.2010.17434.x. ISSN 0035-8711. Bibcode: 2011MNRAS.410..190T.
- ↑ "V2052 Oph -- beta Cep Variable". SIMBAD. Centre de données astronomiques de Strasbourg. http://simbad.u-strasbg.fr/simbad/sim-basic?Ident=V2052+Oph+--+beta+Cep+Variable.
- ↑ Jerzykiewicz, Mikolaj (October 1972). "HR 6684: A New Beta Cephei Type Variable Star". Publications of the Astronomical Society of the Pacific 84 (501): 718–720. doi:10.1086/129368. Bibcode: 1972PASP...84..718J.
- ↑ McNamara, D. H.; Bills, B. G. (October 1973). "Photometric and Spectrographic Observations of HR 6684". Publications of the Astronomical Society of the Pacific 85 (507): 632–636. doi:10.1086/129517. Bibcode: 1973PASP...85..632M.
- ↑ Kukarkin, B. V.; Kholopov, P. N.; Kukarkina, N. P.; Perova, N. B. (October 1973). "59th Name-List of Variable Stars". Information Bulletin on Variable Stars 834: 1. Bibcode: 1973IBVS..834....1K. https://ibvs.konkoly.hu/pub/ibvs/0801/0834.pdf. Retrieved 7 February 2023.
- ↑ Cugier, H.; Dziembowski, W. A.; Pamyatnykh, A. A. (November 1994). "Nonadiabatic observables in β Cephei models". Astronomy and Astrophysics 291: 143–154. Bibcode: 1994A&A...291..143C.
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