Theta1 Orionis A

From Wikipedia, the free encyclopedia
Jump to: navigation, search
θ1 Orionis A
TrapeziumStars.jpg
Trapezium stars
Observation data
Epoch 2000      Equinox 2000
Constellation Orion
Right ascension 05h 35m 15.84743s[1]
Declination −05° 23′ 14.3441″[1]
Apparent magnitude (V) 6.72 - 7.65[2]
Characteristics
Spectral type B0.5V[3]
Variable type Algol[2]
Astrometry
Distance 408 ± 43[3] pc
Absolute magnitude (MV) −2.80[3]
Details
A1
Mass 15.3[3] M
Radius 4.5[3] R
Luminosity 16,200[3] L
Surface gravity (log g) 4.30[3] cgs
Temperature 30,700[3] K
Age <2.5[3] Myr
A3
Mass 2.5 - 2.7[4] M
Radius 6.4[4] R
Details
A2
Mass 4[5] M
Other designations
41 Ori A, V1016 Ori, BD−05 1315A, HD 37020, HIP 26220, HR 1893
Database references
SIMBAD data

Theta1 Orionis A (θ1 Ori A) is a variable trinary star in the constellation Orion. Its apparent magnitude range is 6.72 to 7.65 with a period of 65.432 days. It is one of the main stars in The Trapezium in Orion, along with B, C, and D, as well as the fainter E.

Variability[edit]

θ1 Orionis A varies in brightness, showing dips from magnitude 6.72 to 7.65 every 65.432 days. These are caused by eclipses of a close binary pair. θ1 Orionis A has been assigned the variable star designation V1016 Orionis.[2]

System[edit]

θ1 Orionis A is a star system with three known members. Components A1 and A2 are separated by around 0.2 ", while A1 is itself a spectroscopic binary with two stars separated by about 1 au.

θ1 Orionis A1 is an eclipsing binary but the secondary is not detected in the spectrum and is far less luminous than the primary.[4][6] The secondary has been proposed to be a T Tauri star, possibly of spectral class A.[7][6] The orbit is not well-defined but appears to be eccentric.[4]

θ1 Orionis A2 is approximately one magnitude fainter than A1 and 0.2" away. This corresponds to a projected separation of 90 AU.[7] The relative motion of the two stars has been measured and they are slowly getting closer together but it has not been possible to derive and orbit. The relative motion of the two stars could simply be a straight line, but it is calculated that they are gravitationally bound.[8]

References[edit]

  1. ^ a b Kounkel, Marina; Hartmann, Lee; Loinard, Laurent; Mioduszewski, Amy J.; Dzib, Sergio A.; Ortiz-León, Gisela N.; Rodríguez, Luis F.; Pech, Gerardo; Rivera, Juana L.; Torres, Rosa M.; Boden, Andrew F.; Evans, Neal J.; Briceño, Cesar; Tobin, John (2014). "The Gould's Belt Very Large Array Survey. III. The Orion Region". The Astrophysical Journal. 790: 49. Bibcode:2014ApJ...790...49K. arXiv:1406.1809Freely accessible. doi:10.1088/0004-637X/790/1/49. 
  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 c d e f g h i Nieva, María-Fernanda; Przybilla, Norbert (2014). "Fundamental properties of nearby single early B-type stars". Astronomy & Astrophysics. 566: A7. Bibcode:2014A&A...566A...7N. arXiv:1412.1418Freely accessible. doi:10.1051/0004-6361/201423373. 
  4. ^ a b c d Bossi, M.; Gaspani, A.; Scardia, M.; Tadini, M. (1989). "Orionis A - A pre-main sequence low Q binary system?". Astronomy and Astrophysics (ISSN 0004-6361). 222: 117. Bibcode:1989A&A...222..117B. 
  5. ^ 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. Bibcode:2013A&A...550A..82G. arXiv:1301.3045Freely accessible. doi:10.1051/0004-6361/201220192. 
  6. ^ a b Vitrichenko, E. A.; Klochkova, V. G. (2000). "A Spectroscopic Study of V1016 Ori". Astronomy Letters. 26 (2): 104. Bibcode:2000AstL...26..104V. doi:10.1134/1.20373. 
  7. ^ a b Petr, Monika G.; Coudé Du Foresto, Vincent; Beckwith, Steven V. W.; Richichi, Andrea; McCaughrean, Mark J. (1998). "Binary Stars in the Orion Trapezium Cluster Core". The Astrophysical Journal. 500 (2): 825. Bibcode:1998ApJ...500..825P. doi:10.1086/305751. 
  8. ^ Close, L. M.; Puglisi, A.; Males, J. R.; Arcidiacono, C.; Skemer, A.; Guerra, J. C.; Busoni, L.; Brusa, G.; Pinna, E.; Miller, D. L.; Riccardi, A.; McCarthy, D. W.; Xompero, M.; Kulesa, C.; Quiros-Pacheco, F.; Argomedo, J.; Brynnel, J.; Esposito, S.; Mannucci, F.; Boutsia, K.; Fini, L.; Thompson, D. J.; Hill, J. M.; Woodward, C. E.; Briguglio, R.; Rodigas, T. J.; Briguglio, R.; Stefanini, P.; Agapito, G.; et al. (2012). "High-resolution Images of Orbital Motion in the Orion Trapezium Cluster with the LBT AO System". The Astrophysical Journal. 749 (2): 180. Bibcode:2012ApJ...749..180C. arXiv:1203.2638Freely accessible. doi:10.1088/0004-637X/749/2/180. 

External links[edit]