Theta1 Orionis C
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File:TrapeziumStars.jpg Theta1 Orionis C and companions in the Trapezium cluster | |
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Orion |
| Right ascension | Template:RA[1] |
| Declination | Template:DEC[1] |
| Apparent magnitude (V) | 5.13[2] |
| Characteristics | |
| Spectral type | θ1 Orionis C1: O6Vp[3] θ1 Orionis C2: B0V[4] |
| U−B Template:Engvar | −0.95[2] |
| B−V Template:Engvar | +0.02[2] |
| Variable type | suspected[5] |
| Astrometry | |
| Radial velocity (Rv) | +23.6 ± 2.0[6] km/s |
| Proper motion (μ) | RA: −4.13[1] mas/yr Dec.: 6.82[1] mas/yr |
| Parallax (π) | 2.11±0.41 mas[1] |
| Distance | Script error: No such module "val".[7] pc |
| Absolute magnitude (MV) | −4.9[8] |
| Orbit[7] | |
| Primary | C1 |
| Companion | C2 |
| Period (P) | Script error: No such module "val". yr |
| Semi-major axis (a) | Script error: No such module "val".″ |
| Eccentricity (e) | Script error: No such module "val". |
| Inclination (i) | Script error: No such module "val".° |
| Longitude of the node (Ω) | Script error: No such module "val".° |
| Argument of periastron (ω) (secondary) | Script error: No such module "val".° |
| Details | |
| C1 | |
| Mass | Script error: No such module "val".[4] Template:Solar mass |
| Radius | Script error: No such module "val".[8] Template:Solar radius |
| Luminosity | 204,000[8] Template:Solar luminosity |
| Surface gravity (log g) | 4.1[8] cgs |
| Temperature | Script error: No such module "val".[8] K |
| Rotational velocity (v sin i) | Script error: No such module "val".[8] km/s |
| Age | Script error: No such module "val".[8] Myr |
| C2 | |
| Mass | Script error: No such module "val".[4] Template:Solar mass |
| Metallicity [Fe/H] | {{{metal_fe2}}} dex |
| Other designations | |
| 41 Ori C, HR 1895, HD 37022, SAO 132314, HIP 26221, BD–05°1315C | |
| Database references | |
| SIMBAD | data |
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Theta1 Orionis C (θ1 Orionis C) is a member of the Trapezium open cluster that lies within the Orion Nebula. The star C is the most massive of the four bright stars at the heart of the cluster. It is an O class blue main sequence star with a B-type main sequence companion. Its high luminosity and large distance (about 1,500 light years) give it an apparent visible magnitude of 5.1.
Theta1 Orionis consists of multiple components, primarily the four stars of the Trapezium cluster, all within one arc-minute of each other. Theta2 Orionis is a more distant grouping of three main stars plus several fainter companions, 1-2 arc-minutes from Theta1.
Theta1 C is itself a binary of two massive stars, C1 and C2, plus a very close fainter companion apparently escaping the system.[9]
Theta1 Orionis C1 is responsible for generating most of the ultraviolet light that is slowly ionizing (and perhaps photoevaporating) the Orion Nebula. This UV light is also the primary cause of the glow that illuminates the Orion Nebula. The star emits a powerful stellar wind that is a hundred thousand times stronger than the Sun's, and the outpouring gas moves at 1,000 km/s.
The primary has a strong dipolar magnetic field with an intensity of Script error: No such module "val".. The field is inclined at an angle of Script error: No such module "val". to the rotation axis. Detected in 2002, this was the first O-type star found to have a magnetic field, and is most likely a fossil field. This field is confining the motion of the strong stellar wind, which should reduce the mass loss rate by 80%.[10]
References
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