Theta 1 Orionis B

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Multiple star
Theta 1 Orionis B
Named stars of the trapezoid
Named stars of the trapezoid
AladinLite
Observation
dates equinox :  J2000.0 , epoch : J2000.0
Constellation Orion
Right ascension 05 h 35 m 16.11 s
declination -05 ° 23 ′ 6.9 ″
Apparent brightness 7.96 (7.9 to 8.65) mag
Typing
B − V color index (+0.24) 
U − B color index (−0.49) 
Spectral class B1 V
Variable star type EA 
Astrometry
Radial velocity (26 ± 1) km / s
Proper movement 
Rec. Share: (−0.9 ± 2.1)  mas / a
Dec. portion: (+0.1 ± 1.3)  mas / a
Physical Properties
Dimensions ( 7/4/3/1/2/4 to 6)  M ☉
Other names
and catalog entries
Bayer name Theta 1 Orionis B
Flamsteed name 41 Orionis B
Bonn survey BD −5 ° 1315B
Bright Star Catalog HR 1893 [1]
Henry Draper Catalog HD 37021 [2]
Tycho catalog TYC 4774-954-1 [3]
2MASS catalog 2MASS J05351611-0523068 [4]
Other names BM Orionis

Theta 1 Orionis B ( θ 1 Orionis B , θ 1 Ori B , also 41 Ori B ) is a multiple star system and a member of the trapezoid in the Orion Nebula .

Mini clusters

The Theta 1 Orionis B system probably consists of six or more stars, named B1 to B6, and possibly one more star. The stars seem to be gravitationally bound to each other, but it is believed that this system cannot be stable for a long time. Accordingly, it is expected that the lower-mass components will be thrown out of the system as runaway stars over time .

The masses of the components are very different. The combination of B1, B5 and B6 has the greatest mass with a total of around 14 solar masses . It has long been known that component B1 has a companion B5 only about 0.12 AU away, which makes it an algolstern . In 2018, however, GRAVITY was able to resolve another component B6 at a distance of 3 to 7 AU. The components B2 and B3 are about 50 AU apart (0.12 arc seconds ) and have 4 and 3 solar masses, respectively.

The centers of B1 / B5 / B6 and B2 / B3 are about 0.9 arc seconds apart. The lowest mass in the system seems to have the somewhat remote component B4 with only 1 solar mass. Accordingly, it is also expected that this component will be ejected from the system first.

component Solar masses Spectral
class 		Distance
(AE)
B1 7.2 ± 0.2 B1 V -
B2 4th ? 382 ± 6
B3 3 ? 49 ± 1
B4 1 ? 248 ± 4
B5 2 ? 0.120 ± 0.002
B6 4 to 6 B. 3.5 to 7.2

Web links

Individual evidence

  1. ↑ a b c d e f tet01 Ori B. In: SIMBAD . Center de Données astronomiques de Strasbourg , accessed April 14, 2019 .
  2. ↑ a b V1016 Ori. In: VSX. AAVSO , accessed April 14, 2019 .
  3. ↑ a b c GRAVITY collaboration: Multiple star systems in the Orion nebula . In: Astronomy & Astrophysics . 620, 2018, p. A116. arxiv : 1809.10376 . bibcode : 2018A & A ... 620A.116G . doi : 10.1051 / 0004-6361 / 201833575 .
  4. ↑ a b LM Close, A. Puglisi, JR Males, C. Arcidiacono, A. Skemer, JC Guerra, L. Busoni, G. Brusa, E. Pinna, DL Miller, A. Riccardi, DW McCarthy, M. Xompero, C. Kulesa, F. Quiros-Pacheco, J. Argomedo, J. Brynnel, S. Esposito, F. Mannucci, K. Boutsia, L. Fini, DJ Thompson, JM Hill, CE Woodward, R. Briguglio, TJ Rodigas, R. Briguglio, P. Stefanini, G. Agapito, P. Hinz: High-resolution Images of Orbital Motion in the Orion Trapezium Cluster with the LBT AO System . In: The Astrophysical Journal . 749, No. 2, 2012, p. 180. arxiv : 1203.2638 . bibcode : 2012ApJ ... 749..180C . doi : 10.1088 / 0004-637X / 749/2/180 .
  5. ↑ a b Christine Allen, Rafael Costero, Miroslava Hernández: The Dynamical Future of the mini-cluster θ1 Ori B . In: The Astronomical Journal . 150, No. 6, 2015, p. 167. bibcode : 2015AJ .... 150..167A . doi : 10.1088 / 0004-6256 / 150/6/167 .