Theta1 Orionis D

θ1 Orionis D

Theta1 Orionis D and companions in the Trapezium cluster
Observation data
Epoch J2000      Equinox ICRS
Constellation Orion
Right ascension 05h 35m 17.24645s[1]
Declination −05° 23′ 16.5707″[1]
Apparent magnitude (V) 6.70[2]
Characteristics
Spectral type B1.5V + B[3]
U−B color index −0.71[2]
B−V color index +0.09[2]
Astrometry
Radial velocity (Rv)+32.4[4] km/s
Proper motion (μ) RA: +1.822 mas/yr[1]
Dec.: −0.393 mas/yr[1]
Parallax (π)2.2820±0.0207 mas[1]
Distance1,430 ± 10 ly
(438 ± 4 pc)
Absolute magnitude (MV)−3.3[5]
Orbit[3]
Primaryθ1 Orionis D1
Nameθ1 Orionis D3
Period (P)0.1452 ± 0.0002 years (53.034 ± 0.073 days)
Semi-major axis (a)(1.86±0.06)×10−3"
(0.77±0.03 au)
Eccentricity (e)0.43±0.03
Inclination (i)160±12°
Longitude of the node (Ω)346±24°
Periastron epoch (T)2017.101±0.001
Argument of periastron (ω)
(secondary)		166±27°
Details
θ1 Orionis D1
Mass16±1[3] M☉
Radius5.6±0.8[5] R☉
Luminosity29,500[5] L☉
Surface gravity (log g)4.2±0.1[5] cgs
Temperature32,000±1,000[5] K
Rotational velocity (v sin i)49.0±0.9[5] km/s
Age2.5±0.5[5] Myr
θ1 Orionis D3
Mass6±1[3] M☉
Other designations
θ1 Orionis D, 41 Orionis D, HR 1896, HD 37023, HIP 26224, WDS J05353-0523D
Database references
SIMBADdata

Theta1 Orionis D (θ1 Orionis D) is a binary star system that is part of the Trapezium open cluster that lies within the Orion Nebula.

θ1 Orionis consists of multiple components, primarily the four stars of the Trapezium cluster (A, B, C, and D) all within one arc-minute of each other. θ2 Orionis is a more distant grouping of three main stars plus several fainter companions, 1-2 arc-minutes from θ1.

Characteristics

θ1 D is a spectroscopic binary with an orbital period of 53.03±0.07 d. The two components are named θ1 Orionis D1 and θ1 Orionis D3. D1 is a B-type main-sequence star of spectral type B1.5V and a mass 16 times that of the Sun. D3 is a B-type star, with a mass six times solar and a brightness 1.15 times fainter than the primary in the K-band.[3]

There is a more widely-separated companion 1.4" away (projected separation of 580±10 au), although it is not confirmed to be gravitationally bound. It has an estimated mass of 1.1±0.1 M☉.[3] Infrared Optical Telescope Array observations suggest another companion at 18.6 mas,[6] which was not confirmed with GRAVITY observations.[3]

References

  1. 1 2 3 4 5 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.
  2. 1 2 3 Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237: 0. Bibcode:2002yCat.2237....0D.
  3. 1 2 3 4 5 6 7 GRAVITY Collaboration; Karl, Martina; Pfuhl, Oliver; Eisenhauer, Frank; Genzel, Reinhard; Grellmann, Rebekka; Habibi, Maryam; Abuter, Roberto; Accardo, Matteo; Amorim, António; Anugu, Narsireddy; Ávila, Gerardo; Benisty, Myriam; Berger, Jean-Philippe; Blind, Nicolas (2018-12-01). "Multiple star systems in the Orion nebula". Astronomy and Astrophysics. 620: A116. arXiv:1809.10376. Bibcode:2018A&A...620A.116G. doi:10.1051/0004-6361/201833575. ISSN 0004-6361.
  4. ↑ Olivares, J.; Sánchez, L. J.; Ruelas-Mayorga, A.; Allen, C.; Costero, R.; Poveda, A. (2013). "Kinematics of the Orion Trapezium Based on Diffracto-Astrometry and Historical Data". The Astronomical Journal. 146 (5): 106. arXiv:1310.0769. Bibcode:2013AJ....146..106O. doi:10.1088/0004-6256/146/5/106. S2CID 119110490.
  5. 1 2 3 4 5 6 7 Simón-Díaz, S.; Herrero, A.; Esteban, C.; Najarro, F. (2006). "Detailed spectroscopic analysis of the Trapezium cluster stars inside the Orion nebula". Astronomy and Astrophysics. 448 (1): 351–366. arXiv:astro-ph/0510288. Bibcode:2006A&A...448..351S. doi:10.1051/0004-6361:20053066. ISSN 0004-6361. S2CID 16445304.
  6. ↑ Grellmann, R.; Preibisch, T.; Ratzka, T.; Kraus, S.; Helminiak, K. G.; Zinnecker, H. (2013). "The multiplicity of massive stars in the Orion Nebula Cluster as seen with long-baseline interferometry". Astronomy & Astrophysics. 550: A82. arXiv:1301.3045. Bibcode:2013A&A...550A..82G. doi:10.1051/0004-6361/201220192. S2CID 6554786.
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