VFTS 102

{{Short description|Star in the constellation Dorado}}

{{Starbox begin

| name=VFTS 102

}}

{{Starbox image

| image = 300px

| caption = Artistic depiction of VFTS 102

}}

{{Starbox observe

| epoch = J2000

| constell = Dorado

| ra = {{RA|05|37|39.248}}{{cite journal |bibcode=2003yCat.2246....0C |title=VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) |journal=CDS/ADC Collection of Electronic Catalogues |pages=II/246 |volume=2246 |last1=Cutri |first1=Roc M. |last2=Skrutskie |first2=Michael F. |last3=Van Dyk |first3=Schuyler D. |last4=Beichman |first4=Charles A. |last5=Carpenter |first5=John M. |last6=Chester |first6=Thomas |last7=Cambresy |first7=Laurent |last8=Evans |first8=Tracey E. |last9=Fowler |first9=John W. |last10=Gizis |first10=John E. |last11=Howard |first11=Elizabeth V. |last12=Huchra |first12=John P. |last13=Jarrett |first13=Thomas H. |last14=Kopan |first14=Eugene L. |last15=Kirkpatrick |first15=J. Davy |last16=Light |first16=Robert M. |last17=Marsh |first17=Kenneth A. |last18=McCallon |first18=Howard L. |last19=Schneider |first19=Stephen E. |last20=Stiening |first20=Rae |last21=Sykes |first21=Matthew J. |last22=Weinberg |first22=Martin D. |last23=Wheaton |first23=William A. |last24=Wheelock |first24=Sherry L. |last25=Zacarias |first25=N. |year=2003 |url=http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=II/246 }}

| dec = {{DEC|−69|09|51.04}}

| appmag_v = 15.806{{cite journal|bibcode=2009AJ....138.1003B|arxiv=0905.1328|title=Spitzer SAGE Infrared Photometry of Massive Stars in the Large Magellanic Cloud|journal=The Astronomical Journal|volume=138|issue=4|pages=1003–1021|last1=Bonanos|first1=A. Z.|last2=Massa|first2=D. L.|last3=Sewilo|first3=M.|last4=Lennon|first4=D. J.|last5=Panagia|first5=N.|last6=Smith|first6=L. J.|last7=Meixner|first7=M.|last8=Babler|first8=B. L.|last9=Bracker|first9=S.|last10=Meade|first10=M. R.|last11=Gordon|first11=K. D.|last12=Hora|first12=J. L.|last13=Indebetouw|first13=R.|last14=Whitney|first14=B. A.|year=2009|doi=10.1088/0004-6256/138/4/1003|s2cid=14056495}}

}}

{{Starbox character

| type=Main sequence

| b-v=+0.293

| u-b=−0.879

| class=O9:Vnnne{{cite journal|bibcode=2011ApJ...743L..22D|arxiv=1111.0157|title=The VLT-FLAMES Tarantula Survey: The Fastest Rotating O-type Star and Shortest Period LMC Pulsar—Remnants of a Supernova Disrupted Binary?|journal=The Astrophysical Journal Letters|volume=743|pages=L22|last1=Dufton|first1=P. L.|last2=Dunstall|first2=P. R.|last3=Evans|first3=C. J.|last4=Brott|first4=I.|last5=Cantiello|first5=M.|last6=De Koter|first6=A.|last7=De Mink|first7=S. E.|author7-link=Selma de Mink|last8=Fraser|first8=M.|last9=Hénault-Brunet|first9=V.|last10=Howarth|first10=I. D.|last11=Langer|first11=N.|last12=Lennon|first12=D. J.|last13=Markova|first13=N.|last14=Sana|first14=H.|last15=Taylor|first15=W. D.|year=2011|issue=1|doi=10.1088/2041-8205/743/1/L22|s2cid=118448435}}

}}

{{Starbox astrometry

| radial_v=228

| prop_mo_ra=7.3

| prop_mo_dec=2.1

| dist_ly = 164,000

| dist_pc = 50,000

| absmag_v=

}}

{{Starbox detail

| source=

| mass={{nowrap|~ 25}}

| rotational_velocity=610±30{{cite journal|title=HST/COS Spectra of the Wind Lines of VFTS 102 and 285|journal=The Astrophysical Journal|first1=Katherine|last1=Shepard|volume=888|number=2|date=January 2020|pages=82|doi=10.3847/1538-4357/ab5a82|arxiv=1911.09675|bibcode=2020ApJ...888...82S|s2cid=208202016 |doi-access=free }}

| luminosity={{nowrap|100,000}}

| temperature={{nowrap|36,000 ± 5000}}

| gravity={{nowrap|3.6 ± 0.5}}

}}

{{Starbox catalog

| names=2MASS J05373924-6909510

}}

{{Starbox reference

|Simbad=VFTS+102

}}

{{Starbox end}}

File:VFTS 102.jpg

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 ~{{val|610|ul=km/s}} (about {{val|2,000,000|ul=km/h|fmt=commas}}), making it the second fastest rotating massive star known alongside VFTS 285 ({{val|609|u=km/s}}), and preceded only by the WO star WR 142 which has a rotational velocity of {{val|1000|ul=km/s}}.{{cite journal|bibcode=2013MNRAS.428.1218J|arxiv=1302.6296|title=The binary merger channel for the progenitor of the fastest rotating O-type star VFTS 102|journal=Monthly Notices of the Royal Astronomical Society|volume=428|issue=2|pages=1218|last1=Jiang|first1=Dengkai|last2=Han|first2=Zhanwen|last3=Yang|first3=Liheng|last4=Li|first4=Lifang|year=2013|doi=10.1093/mnras/sts105|doi-access=free |s2cid=118856665}}{{Cite journal|last1=Sander|first1=A.|last2=Hamann|first2=W.-R.|last3=Todt|first3=H.|date=April 2012|title=The Galactic WC stars. Stellar parameters from spectral analyses indicate a new evolutionary sequence|url=https://ui.adsabs.harvard.edu/abs/2012A&A...540A.144S/abstract|journal=Astronomy and Astrophysics|language=en|volume=540|pages=A144|doi=10.1051/0004-6361/201117830|issn=0004-6361|arxiv=1201.6354|bibcode=2012A&A...540A.144S|s2cid=119182468}} 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.{{cite journal|bibcode=2007A&A...465L..29C|title=Binary star progenitors of long gamma-ray bursts|journal=Astronomy and Astrophysics|volume=465|issue=2|pages=L29|last1=Cantiello|first1=M.|last2=Yoon|first2=S.-C.|last3=Langer|first3=N.|last4=Livio|first4=M.|year=2007|doi=10.1051/0004-6361:20077115|arxiv = astro-ph/0702540 |s2cid=118921504}}