Astronomy:Theta2 Orionis

From HandWiki
Short description: Star in the constellation Orion


θ2 Orionis
Theta2Orionis.jpg
The three components of θ2 Orionis, plus nearby stars
Credit: Ian Nartowicz (derived from ESA/Hubble image)
Observation data
{{#ifeq:J2000|J2000.0 (ICRS)|Epoch J2000.0      Equinox J2000.0 (ICRS)| Epoch J2000      [[Astronomy:Equinox (celestial coordinates)|Equinox J2000}}
Constellation Orion
A
Right ascension  05h 35m 22.90124s[1]
Declination −05° 24′ 57.8326″[1]
Apparent magnitude (V) 5.02[2]
B
Right ascension  05h 35m 26.40075s[3]
Declination −05° 25′ 00.7938″[3]
Apparent magnitude (V) 6.380[4]
C
Right ascension  05h 35m 31.43111s[5]
Declination −05° 25′ 16.3717″[5]
Apparent magnitude (V) 8.18[6]
Characteristics
Spectral type O9.5IVp[7] + B0.7V[8] + B5V[9]
Astrometry
A
Radial velocity (Rv)35.6[10] km/s
Proper motion (μ) RA: +2.630[1] mas/yr
Dec.: +2.394[1] mas/yr
Parallax (π)2.9728 ± 0.2136[1] mas
Distance1,100 ± 80 ly
(340 ± 20 pc)
Absolute magnitude (MV)−4.3[11]
B
Proper motion (μ) RA: +1.161[3] mas/yr
Dec.: +0.162[3] mas/yr
Parallax (π)2.3870 ± 0.0499[3] mas
Distance1,370 ± 30 ly
(419 ± 9 pc)
Absolute magnitude (MV)−2.60[4]
C
Proper motion (μ) RA: +2.510[5] mas/yr
Dec.: +3.731[5] mas/yr
Parallax (π)2.4513 ± 0.0380[5] mas
Distance1,330 ± 20 ly
(408 ± 6 pc)
Absolute magnitude (MV)−0.6[12]
Details
A
Mass39[13] M☉
Luminosity107,000[14] L☉
Temperature34,900[14] K
Rotational velocity (v sin i)133[8] km/s
B
Mass14.8[4] M☉
Radius4.3[4] R☉
Luminosity12,300[4] L☉
Surface gravity (log g)4.30[4] cgs
Temperature29,300[4] K
Rotational velocity (v sin i)33[8] km/s
Age<2[4] Myr
C
Mass4.86[14] M☉
Luminosity616[14] L☉
Temperature13,800[14] K
Rotational velocity (v sin i)78[15] km/s
Age<1[15] Myr
Other designations
θ2 Ori, STF 4016, WDS J05354-0525, ADS 4188
θ2 Ori A: 43 Ori, HR 1897, BD−05°1319, HD 37041, SAO 132321, HIP 26235, CCDM 05353-0524E
θ2 Ori B: BD−05°1320, HD 37042, SAO 132322, CCDM 05353-0524F
θ2 Ori C: V361 Ori, BD−05°1326, HD 37062, SAO 132329, S 490A, CCDM 05353-0524G
Database references
SIMBADdata
data2
data3

Theta2 Orionis (θ2 Ori) is a multiple star system in the constellation Orion. It is a few arc minutes from its more famous neighbour the Trapezium Cluster, also known as θ1 Orionis.

Components

The three stars of θ2 Orionis within the Orion Nebula

θ2 Orionis consists of three stars in a line, each about an arc-minute from the next. In addition to the well-known three stars, the Washington Double Star Catalog confusingly lists a component D which is actually θ1 Orionis C.[16]

There is one other star brighter than 10th magnitude in the region. V1073 Orionis is a B9.5 Orion variable that forms an equilateral triangle with θ2 Ori B and C.

Bizarrely, θ2 Orionis C has a second entry in the Washington Double Star Catalog under the name S490. The companion is 10th magnitude and actually lies between θ2 Ori B and V1073 Ori.[16]

θ1 Orionis, the well known Trapezium cluster, is only 2 arc minutes away from θ2 Orionis A. Despite the names, θ2 Orionis A is marginally brighter than the brightest star in the Trapezium. The Catalog of Components of Double and Multiple Stars includes the stars of θ1 and θ2 Ori within the same system of 13 components.

There are dozens of much fainter stars in the same field, many of them pre-main-sequence stars still forming from the Orion molecular cloud complex.

Properties

The primary component A appears as a 5th magnitude O class subgiant over 100,000 times as luminous as the sun. The spectral type suggests it is evolving away from the main sequence, although it is thought to be less than 2 million years old. The spectral peculiarities may be related to close companions or could be caused by the extreme youth of the star.

The 6th magnitude component B is an early B main sequence star nearly 30,000 K and over 10,000 times the luminosity of the sun.

Component C is another B class main sequence star, but cooler and less than a thousand times the luminosity of the sun.

θ2 Orionis A system

θ2 Orionis A is itself a triple star system. Its spectral lines were seen to change position periodically, indicating orbital motion. The first orbit was derived in 1924, indicating a period of 21 days. and a rather eccentric orbit.[17]

Speckle interferometry has resolved a companion about 0.3" away, around 147 AU. High resolution spectroscopy shows that there is an even closer companion, only about 0.47 AU from the primary, for a total of three stars. Both companions are thought to be early A or late B with masses of 7-9 M☉. This helps to explain the high mass and visual luminosity for an O9.5 star at this distance. The three stars together have nearly the same mass as the O5.5 θ1 Orionis C and visually are even brighter.[18]

θ2 Orionis A also shows unexplained rapidly variable x-ray emission. The x-rays cannot be explained standard mechanisms such as colliding winds or coronal emissions from an unseen companion.[13]

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 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.
  2. ↑ Aldoretta, E. J.; Caballero-Nieves, S. M.; Gies, D. R.; Nelan, E. P.; Wallace, D. J.; Hartkopf, W. I.; Henry, T. J.; Jao, W.-C. et al. (2015). "The Multiplicity of Massive Stars: A High Angular Resolution Survey with the Guidance Sensor". The Astronomical Journal 149 (1): 26. doi:10.1088/0004-6256/149/1/26. Bibcode: 2015AJ....149...26A. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 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.
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 Nieva, María-Fernanda; Przybilla, Norbert (2014). "Fundamental properties of nearby single early B-type stars". Astronomy & Astrophysics 566: A7. doi:10.1051/0004-6361/201423373. Bibcode: 2014A&A...566A...7N. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 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.
  6. ↑ Pasinetti Fracassini, L. E.; Pastori, L.; Covino, S.; Pozzi, A. (2001). "Catalogue of Apparent Diameters and Absolute Radii of Stars (CADARS) - Third edition - Comments and statistics". Astronomy and Astrophysics 367 (2): 521. doi:10.1051/0004-6361:20000451. Bibcode: 2001A&A...367..521P. 
  7. ↑ Sota, A.; Maíz Apellániz, J.; Walborn, N. R.; Alfaro, E. J.; Barbá, R. H.; Morrell, N. I.; Gamen, R. C.; Arias, J. I. (2011). "The Galactic O-Star Spectroscopic Survey. I. Classification System and Bright Northern Stars in the Blue-violet at R ~ 2500". The Astrophysical Journal Supplement 193 (2): 24. doi:10.1088/0067-0049/193/2/24. Bibcode: 2011ApJS..193...24S. 
  8. ↑ 8.0 8.1 8.2 Simón-Díaz, S.; Herrero, A. (2014). "The IACOB project. I. Rotational velocities in northern Galactic O- and early B-type stars revisited. The impact of other sources of line-broadening". Astronomy & Astrophysics 562: A135. doi:10.1051/0004-6361/201322758. Bibcode: 2014A&A...562A.135S. 
  9. ↑ Houk, N.; Swift, C. (1999). "Michigan catalogue of two-dimensional spectral types for the HD Stars, Vol. 5". Michigan Spectral Survey 05: 0. Bibcode: 1999MSS...C05....0H. 
  10. ↑ Wilson, Ralph Elmer (1953). "General catalogue of stellar radial velocities". Washington. Bibcode: 1953GCRV..C......0W. 
  11. ↑ Abbott, D. C. (1978). "The terminal velocities of stellar winds from early-type stars". Astrophysical Journal 225: 893. doi:10.1086/156554. Bibcode: 1978ApJ...225..893A. 
  12. ↑ Abt, H. A. (1979). "The occurrence of abnormal stars in open clusters". Astrophysical Journal 230: 485. doi:10.1086/157104. Bibcode: 1979ApJ...230..485A. 
  13. ↑ 13.0 13.1 Mitschang, Arik W.; Schulz, Norbert S.; Huenemoerder, David P.; Nichols, Joy S.; Testa, Paola (2011). "Detailed X-Ray Line Properties of θ2 Ori a in Quiescence". The Astrophysical Journal 734 (1): 14. doi:10.1088/0004-637X/734/1/14. Bibcode: 2011ApJ...734...14M. 
  14. ↑ 14.0 14.1 14.2 14.3 14.4 Hillenbrand, Lynne A. (1997). "On the Stellar Population and Star-Forming History of the Orion Nebula Cluster". Astronomical Journal 113: 1733. doi:10.1086/118389. Bibcode: 1997AJ....113.1733H. 
  15. ↑ 15.0 15.1 Manoj, P.; Maheswar, G.; Bhatt, H. C. (2002). "Non-emission-line young stars of intermediate mass". Monthly Notices of the Royal Astronomical Society 334 (2): 419. doi:10.1046/j.1365-8711.2002.05540.x. Bibcode: 2002MNRAS.334..419M. 
  16. ↑ 16.0 16.1 Mason, Brian D.; Wycoff, Gary L.; Hartkopf, William I.; Douglass, Geoffrey G.; Worley, Charles E. (2001). "The 2001 US Naval Observatory Double Star CD-ROM. I. The Washington Double Star Catalog". The Astronomical Journal 122 (6): 3466. doi:10.1086/323920. Bibcode: 2001AJ....122.3466M. 
  17. ↑ Struve, O. (1924). "The orbit of the spectroscopic binary 43 theta-2 Orionis". Astrophysical Journal 60: 159. doi:10.1086/142845. Bibcode: 1924ApJ....60..159S. 
  18. ↑ Schulz, Norbert S.; Testa, Paola; Huenemoerder, David P.; Ishibashi, Kazunori; Canizares, Claude R. (2006). "X-Ray Variability in the Young Massive Triple θ2 Orionis A". The Astrophysical Journal 653 (1): 636–646. doi:10.1086/508625. Bibcode: 2006ApJ...653..636S. 



Retrieved from "https://handwiki.org/wiki/index.php?title=Astronomy:Theta2_Orionis&oldid=3427760"