Astronomy:R145
.jpg) R145 is the isolated bright star to the left of the image, near R136 (annotated at Commons) Credit: NASA, ESA, F. Paresce (INAF-IASF, Bologna, Italy), R. O'Connell (University of Virginia, Charlottesville), and the Wide Field Camera 3 Science Oversight Committee | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Dorado |
| Right ascension | 05h 38m 57.059s[1] |
| Declination | −69° 06′ 05.70″[1] |
| Apparent magnitude (V) | 12.04[2] |
| Characteristics | |
| Spectral type | WN6h + O3.5If*/WN7[3] |
| U−B color index | −0.79[4] |
| B−V color index | −0.01[2] |
| Astrometry | |
| Radial velocity (Rv) | 270 ± 5[3] km/s |
| Distance | 163,000 ly (49,970[5] pc) |
| Absolute magnitude (MV) | −7.21 + −7.43[3] |
| Orbit[3] | |
| Period (P) | 158.760 |
| Semi-major axis (a) | 955 R☉ |
| Eccentricity (e) | 0.788 ± 0.007 |
| Inclination (i) | 39 ± 6° |
| Semi-amplitude (K1) (primary) | 96 ± 3 km/s |
| Semi-amplitude (K2) (secondary) | 95 ± 4 km/s |
| Details[3] | |
| Primary | |
| Mass | 53+40 −20 M☉ |
| Radius | 20+6 −5 R☉ |
| Luminosity | 2,240,000+924,000 −654,000 L☉ |
| Temperature | 50,000 ± 3,000 K |
| Rotational velocity (v sin i) | < 200 km/s |
| Secondary | |
| Mass | 54+40 −20 M☉ |
| Radius | 26+9 −7 R☉ |
| Luminosity | 2,140,000+882,000 −624,000 L☉ |
| Temperature | 43,000 ± 3,000 K |
| Rotational velocity (v sin i) | < 150 km/s |
| Age | 2.2 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
R145 (HD 269928) is a spectroscopic binary star in the Tarantula Nebula in the Large Magellanic Cloud located in the constellation Dorado. Both components are amongst the most luminous known.
Observations
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R145 is listed in the Henry Draper Catalogue with photographic magnitude 11.8. The spectral type is given as O which then included all types of hot stars showing emission lines. It is included in the first Henry Draper Extension volume published in 1925.[6]
In 1960 R145 was included in the Radcliffe Magellanic Catalogue of the brightest stars in the Magellanic Clouds with a somewhat uncertain WN6-7 spectral type. Stars in the catalogue are referred to by the acronym RMC and their catalogue entry number, or just R with the number.[7]
In the first catalogue of LMC Wolf-Rayet stars, R145 is listed as number 90 with spectral type WN7. Stars in this catalogue are referred to with the abbreviation Brey after the author Breysacher.[8] In the fourth catalogue published in 1999, it is listed as BAT99-119.[9]
In the Very Large Telescope FLAMES survey published in 2011, R145 was given the designation VFTS 695. It was given the spectral type WN6h to recognise that it retained a significant amount of hydrogen in its atmosphere. It was also recognised that there was a second luminous star in the system but a spectral type could not be determined for it.[10]
In 2016, the orbit and physical parameters of the two stars were calculated from FLAMES survey data.[3]
System
R145 is a double-lined spectroscopic binary system with an orbital period of 159 days. The two stars have an eccentric orbit with a separation varying from less than one AU to nearly eight AU. They have almost identical orbital velocities and hence very similar masses. The exact values depend on the inclination of the orbital plane. The inclination of the R145 orbit calculated using polarimetry is 39°. At this small inclination the formal error of 6° translates into considerable margins of error in the masses. Estimates of the masses of the two stars by other methods give larger values, suggesting that the inclination may be smaller than 39°.[3]
Components
The primary component of R145 is designated as the star which dominates the spectrum with its strong broad emission lines. It is a WN6h Wolf-Rayet star with a temperature of around 50,000 K. Although it has a WR spectral type, it is a relatively young star which still has about 40% hydrogen in its atmosphere. The atmospheric enhancement of helium and nitrogen is caused by strong convection and heavy mass loss produced by the high luminosity and probably by rapid rotation.[3]
The secondary component is actually marginally more massive and visually brighter than the primary. It has a lower temperature of about 43,000 K and a larger size at 26 R☉. Its bolometric. Its spectral type is given as O3.5If*/WN7. The bolometric luminosity of each star is over two million times greater than the sun.[3]
The masses of the primary and secondary determined from the calculated orbit are 53 M☉ and 54 M☉ respectively, but these depend strongly on the precise orbital inclination and both the masses are likely to be somewhere between 23 M☉ and 94 M☉. Calculation of spectral and evolutionary masses suggest that the two masses are both near 80 M☉. Then the ages of the stars are about 2.2 million years and their initial masses were 105 M☉ and 90 M☉.[3]
References
- ↑ 1.0 1.1 Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P. et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27. doi:10.1888/0333750888/2862. ISBN 0333750888. Bibcode: 2000A&A...355L..27H.
- ↑ 2.0 2.1 Doran, E. I.; Crowther, P. A.; De Koter, A.; Evans, C. J.; McEvoy, C.; Walborn, N. R.; Bastian, N.; Bestenlehner, J. M. et al. (2013). "The VLT-FLAMES Tarantula Survey. XI. A census of the hot luminous stars and their feedback in 30 Doradus". Astronomy & Astrophysics 558: A134. doi:10.1051/0004-6361/201321824. Bibcode: 2013A&A...558A.134D.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 3.8 3.9 Shenar, T. (2016). "The Tarantula Massive Binary Monitoring project: II. A first SB2 orbital and spectroscopic analysis for the Wolf-Rayet binary R145". Astronomy & Astrophysics 598: A85. doi:10.1051/0004-6361/201629621. Bibcode: 2017A&A...598A..85S.
- ↑ Feitzinger, J. V.; Isserstedt, J. (1983). "Photoelectric UBV-photometry of Wolf-Rayet stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement Series 51: 505. Bibcode: 1983A&AS...51..505F.
- ↑ Pietrzyński, G et al. (7 March 2013). "An eclipsing-binary distance to the Large Magellanic Cloud accurate to two per cent". Nature 495 (7439): 76–79. doi:10.1038/nature11878. PMID 23467166. Bibcode: 2013Natur.495...76P.
- ↑ Cannon, A. J. (1925). "The Henry Draper extension". Annals of the Astronomical Observatory of Harvard College 100: 17. Bibcode: 1925AnHar.100...17C.
- ↑ Feast, M. W.; Thackeray, A. D.; Wesselink, A. J. (1960). "The brightest stars in the Magellanic Clouds". Monthly Notices of the Royal Astronomical Society 121 (4): 337–385. doi:10.1093/mnras/121.4.337. Bibcode: 1960MNRAS.121..337F.
- ↑ Breysacher, J. (1981). "Spectral Classification of Wolf-Rayet Stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement 43: 203. Bibcode: 1981A&AS...43..203B.
- ↑ Breysacher, J.; Azzopardi, M.; Testor, G. (1999). "The fourth catalogue of Population I Wolf-Rayet stars in the Large Magellanic Cloud". Astronomy and Astrophysics Supplement 137: 117–145. doi:10.1051/aas:1999240. Bibcode: 1999A&AS..137..117B.
- ↑ Evans, C. J.; Taylor, W. D.; Hénault-Brunet, V.; Sana, H.; De Koter, A.; Simón-Díaz, S.; Carraro, G.; Bagnoli, T. et al. (2011). "The VLT-FLAMES Tarantula Survey. I. Introduction and observational overview". Astronomy & Astrophysics 530: A108. doi:10.1051/0004-6361/201116782. Bibcode: 2011A&A...530A.108E.
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