VFTS 102

VFTS 102

Artistic depiction of VFTS 102
Observation data
Epoch J2000      Equinox J2000
Constellation Dorado
Right ascension 05h 37m 39.248s[1]
Declination −69° 09′ 51.04″[1]
Apparent magnitude (V) 15.806[2]
Characteristics
Evolutionary stage Main sequence
Spectral type O9:Vnnne[3]
U−B color index −0.879[2]
B−V color index +0.293[2]
Astrometry
Radial velocity (Rv)228[3] km/s
Proper motion (μ) RA: 7.3[1] mas/yr
Dec.: 2.1[1] mas/yr
Distance164,000 ly
(50,000 pc)
Details[3]
Mass~ 25 M☉
Luminosity100,000 L☉
Surface gravity (log g)3.6 ± 0.5 cgs
Temperature36,000 ± 5000 K
Rotational velocity (v sin i)610±30[4] km/s
Other designations
2MASS J05373924-6909510
Database references
SIMBADdata
The position of VFTS 102 in Tarantula nebula

VFTS 102 is a star located in the Tarantula nebula, a star forming region in the Large Magellanic Cloud, a satellite galaxy of the Milky Way.

The peculiarity of this star is its projected equatorial velocity of ~610 km/s (about 2,000,000 km/h), making it the second fastest rotating massive star known alongside VFTS 285 (609 km/s), and preceded only by the WO star WR 142 which has a rotational velocity of 1000 km/s.[4][5][6] The resulting centripetal force tends to flatten the star; material can be lost in the loosely bound equatorial regions, allowing for the formation of a disk. The spectroscopic observations seem to confirm this, and the star is classified as Oe, possibly due to emission from such an equatorial disk of gas.

This star was observed by the VLT Flames Tarantula Survey collaboration using the VLT, Very Large Telescope in Chile. One member of this team is Matteo Cantiello, an Italian astrophysicist who emigrated to the United States and is currently working at the Kavli Institute for Theoretical Physics at University of California Santa Barbara. In 2007, together with a few collaborators, he predicted the existence of massive stars with properties very similar to VFTS 102. In its theoretical model, the extreme rotational speed is caused by the transfer of material from a companion star in a binary system. After this "cosmic dance", the donor star is predicted to explode as a supernova. The spun-up companion instead is likely to be launched out of the orbit and move away from its stellar neighbors at high speed. Such a star is called a runaway. VFTS 102 fits this theoretical model very well, being found to be a rapidly rotating runaway star and lying close to a pulsar and a supernova remnant. Other scenarios, like a dynamical ejection from the core of the star cluster R136, are also possible.[7]

References

  1. ^ a b c d Cutri, Roc M.; Skrutskie, Michael F.; Van Dyk, Schuyler D.; Beichman, Charles A.; Carpenter, John M.; Chester, Thomas; Cambresy, Laurent; Evans, Tracey E.; Fowler, John W.; Gizis, John E.; Howard, Elizabeth V.; Huchra, John P.; Jarrett, Thomas H.; Kopan, Eugene L.; Kirkpatrick, J. Davy; Light, Robert M.; Marsh, Kenneth A.; McCallon, Howard L.; Schneider, Stephen E.; Stiening, Rae; Sykes, Matthew J.; Weinberg, Martin D.; Wheaton, William A.; Wheelock, Sherry L.; Zacarias, N. (2003). "VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)". CDS/ADC Collection of Electronic Catalogues. 2246: II/246. Bibcode:2003yCat.2246....0C.
  2. ^ a b c Bonanos, A. Z.; Massa, D. L.; Sewilo, M.; Lennon, D. J.; Panagia, N.; Smith, L. J.; Meixner, M.; Babler, B. L.; Bracker, S.; Meade, M. R.; Gordon, K. D.; Hora, J. L.; Indebetouw, R.; Whitney, B. A. (2009). "Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud". The Astronomical Journal. 138 (4): 1003–1021. arXiv:0905.1328. Bibcode:2009AJ....138.1003B. doi:10.1088/0004-6256/138/4/1003. S2CID 14056495.
  3. ^ a b c Dufton, P. L.; Dunstall, P. R.; Evans, C. J.; Brott, I.; Cantiello, M.; De Koter, A.; De Mink, S. E.; Fraser, M.; Hénault-Brunet, V.; Howarth, I. D.; Langer, N.; Lennon, D. J.; Markova, N.; Sana, H.; Taylor, W. D. (2011). "The VLT-FLAMES Tarantula Survey: The Fastest Rotating O-type Star and Shortest Period LMC Pulsar—Remnants of a Supernova Disrupted Binary?". The Astrophysical Journal Letters. 743 (1): L22. arXiv:1111.0157. Bibcode:2011ApJ...743L..22D. doi:10.1088/2041-8205/743/1/L22. S2CID 118448435.
  4. ^ a b Shepard, Katherine (January 2020). "HST/COS Spectra of the Wind Lines of VFTS 102 and 285". The Astrophysical Journal. 888 (2): 82. arXiv:1911.09675. Bibcode:2020ApJ...888...82S. doi:10.3847/1538-4357/ab5a82. S2CID 208202016.
  5. ^ Jiang, Dengkai; Han, Zhanwen; Yang, Liheng; Li, Lifang (2013). "The binary merger channel for the progenitor of the fastest rotating O-type star VFTS 102". Monthly Notices of the Royal Astronomical Society. 428 (2): 1218. arXiv:1302.6296. Bibcode:2013MNRAS.428.1218J. doi:10.1093/mnras/sts105. S2CID 118856665.
  6. ^ Sander, A.; Hamann, W.-R.; Todt, H. (April 2012). "The Galactic WC stars. Stellar parameters from spectral analyses indicate a new evolutionary sequence". Astronomy and Astrophysics. 540: A144. arXiv:1201.6354. Bibcode:2012A&A...540A.144S. doi:10.1051/0004-6361/201117830. ISSN 0004-6361. S2CID 119182468.
  7. ^ Cantiello, M.; Yoon, S.-C.; Langer, N.; Livio, M. (2007). "Binary star progenitors of long gamma-ray bursts". Astronomy and Astrophysics. 465 (2): L29. arXiv:astro-ph/0702540. Bibcode:2007A&A...465L..29C. doi:10.1051/0004-6361:20077115. S2CID 118921504.