11 Orionis

Nowadays, 11 Orionis has become an increasingly relevant topic of debate in our society. Since its emergence, 11 Orionis has captured the attention of experts and the general public, generating mixed opinions and passionate discussions. Over time, 11 Orionis has proven its importance in different areas, from politics to technology, culture and education. In this article, we will explore the most relevant aspects of 11 Orionis and its impact on daily life, as well as the possible implications it could have in the future.

11 Orionis
Location of 11 Orionis (circled)
Observation data
Epoch J2000      Equinox J2000
Constellation Orion
Right ascension 05h 04m 34.14916s[1]
Declination +15° 24′ 14.7771″[1]
Apparent magnitude (V) [2] 4.65
Characteristics
Spectral type B9 IV[3] or A1 Vp SiCr[4]
U−B color index −0.10[5]
B−V color index −0.06[5]
Variable type α² CVn[2]
Astrometry
Radial velocity (Rv)+16.80[6] km/s
Proper motion (μ) RA: +17.80[1] mas/yr
Dec.: −31.15[1] mas/yr
Parallax (π)8.93±0.24 mas[1]
Distance365 ± 10 ly
(112 ± 3 pc)
Absolute magnitude (MV)−0.59[7]
Details
Mass2.7[8] M☉
Radius4.3[8] R☉
Luminosity220[7] L☉
Surface gravity (log g)3.6[8] cgs
Temperature9,520[3] K
Rotational velocity (v sin i)63.3±3.6[8] km/s
Other designations
11 Ori, V1032 Ori, BD+15°732, FK5 1140, GC 6191, HD 32549, HIP 23607, HR 1638, SAO 94290[9]
Database references
SIMBADdata

11 Orionis is a solitary[10] Ap star in the equatorial constellation of Orion, near the border with Taurus. It is visible to the naked eye with an apparent visual magnitude of 4.65,[7] and it is located approximately 365 light years away from the Sun based on parallax.[1] The star is moving further from the Sun with a heliocentric radial velocity of +16.8 km/s.[6]

A light curve for V1032 Orionis, plotted from TESS data[11]

This object is a chemically peculiar star, known as an Ap star, with enhanced silicon and chromium lines in its spectrum.[12] It is an α² CVn variable, ranging from 4.65 to 4.69 magnitude with a period of 4.64 days.[2] The magnetic field measured from metal lines has a strength of +160±390 G.[13]

References

  1. ^ a b c d e f Van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics. 474 (2): 653–664. arXiv:0708.1752. Bibcode:2007A&A...474..653V. doi:10.1051/0004-6361:20078357. S2CID 18759600. Vizier catalog entry
  2. ^ a b c 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.
  3. ^ a b Zorec, J.; Cidale, L.; Arias, M. L.; Frémat, Y.; Muratore, M. F.; Torres, A. F.; Martayan, C. (2009). "Fundamental parameters of B supergiants from the BCD system. I. Calibration of the (λ_1, D) parameters into Teff". Astronomy and Astrophysics. 501 (1): 297–320. arXiv:0903.5134. Bibcode:2009A&A...501..297Z. doi:10.1051/0004-6361/200811147. S2CID 14969137.
  4. ^ Abt, Helmut A.; Morrell, Nidia I. (1995). "The Relation between Rotational Velocities and Spectral Peculiarities among A-Type Stars". Astrophysical Journal Supplement. 99: 135. Bibcode:1995ApJS...99..135A. doi:10.1086/192182.
  5. ^ a b Mermilliod, J. C. (2006). "VizieR Online Data Catalog: Homogeneous Means in the UBV System (Mermilliod 1991)". VizieR On-line Data Catalog: II/168. Originally Published in: Institut d'Astronomie. 2168. Bibcode:2006yCat.2168....0M.Vizier catalog entry
  6. ^ a b Wilson, R. E. (1953). "General Catalogue of Stellar Radial Velocities". Carnegie Institute Washington D.C. Publication. Carnegie Institution for Science. Bibcode:1953GCRV..C......0W. ISBN 9780598216885. LCCN 54001336.
  7. ^ 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. Vizier catalog entry
  8. ^ a b c d Moiseeva, A. V.; et al. (January 2019). "Fundamental Parameters of CP Stars Observed at the 6-m Telescope. I. Observations in 2009–2011". Astrophysical Bulletin. 74 (1): 62–65. Bibcode:2019AstBu..74...62M. doi:10.1134/S1990341319010061.
  9. ^ "11 Ori". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 8 September 2012.
  10. ^ Eggleton, P. P.; Tokovinin, A. A. (September 2008). "A catalogue of multiplicity among bright stellar systems". Monthly Notices of the Royal Astronomical Society. 389 (2): 869–879. arXiv:0806.2878. Bibcode:2008MNRAS.389..869E. doi:10.1111/j.1365-2966.2008.13596.x. S2CID 14878976.
  11. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  12. ^ Stigler, Ch.; Maitzen, H. M.; Paunzen, E.; Netopil, M. (2014). "Spectrophotometric analysis of the 5200 Å region for peculiar and normal stars". Astronomy & Astrophysics. 562: A65. arXiv:1402.1021. Bibcode:2014A&A...562A..65S. doi:10.1051/0004-6361/201322300. S2CID 55166743.
  13. ^ Romanyuk, I. I.; et al. (July 2016). "Results of magnetic field measurements of CP-stars performed with the 6-m telescope. III. Observations in 2009". Astrophysical Bulletin. 71 (3): 302–313. Bibcode:2016AstBu..71..302R. doi:10.1134/S1990341316030056. S2CID 125202761.