Astronomy:HVS 7
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Leo |
| Right ascension | 11h 33m 12.125s[1] |
| Declination | +01° 08′ 24.87″[1] |
| Apparent magnitude (V) | 17.80[2] |
| Characteristics | |
| Spectral type | sdB[3] |
| Astrometry | |
| Radial velocity (Rv) | 518[4] km/s |
| Proper motion (μ) | RA: -1[5] mas/yr Dec.: 1[5] mas/yr |
| Distance | 180,000 ly (55,000[6] pc) |
| Details[7] | |
| Mass | 3.7 M☉ |
| Radius | 4.0 R☉ |
| Luminosity | 300 L☉ |
| Surface gravity (log g) | 3.8 cgs |
| Temperature | 12,000 K |
| Rotational velocity (v sin i) | 55 km/s |
| Age | 150 Myr |
| Other designations | |
| Database references | |
| SIMBAD | data |
HVS 7 -- hyper-velocity star 7, otherwise known as SDSS J113312.12+010824.9 is a rare star that has been accelerated to faster than our Milky Way Galaxy's escape velocity.[7][8] In 2013 a team under N. Przybilla wrote that the star had a chemically peculiar photosphere, which masked its origins.[7] The star was first cataloged during the Sloan Digital Sky Survey. It was identified as a hyper-velocity star in 2006.[8]
The star has a chemically peculiar spectrum, roughly matching a B-type subdwarf. Stars in this region of the Hertzsprung–Russell diagram are expected to either be hot horizontal branch stars, low-mass helium-burning objects, or moderate mass hydrogen-burning stars slightly below the main sequence. The high rotational velocity of HVS 7 means it is likely to be a young star near the main sequence, around 150 million years old and 3.7 times the mass of the sun.[7]
References
- ↑ 1.0 1.1 Adelman-McCarthy, Jennifer K. (2008). "The Sixth Data Release of the Sloan Digital Sky Survey". The Astrophysical Journal Supplement Series 175 (2): 297–313. doi:10.1086/524984. Bibcode: 2008ApJS..175..297A.
- ↑ Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.; Kurtz, Michael J.; Bromley, Benjamin C. (2007). "Hypervelocity Stars. III. The Space Density and Ejection History of Main-Sequence Stars from the Galactic Center". The Astrophysical Journal 671 (2): 1708. doi:10.1086/523642. Bibcode: 2007ApJ...671.1708B.
- ↑ Harris, Hugh C.; Liebert, James; Kleinman, S. J.; Nitta, Atsuko; Anderson, Scott F.; Knapp, Gillian R.; Krzesiński, Jurek; Schmidt, Gary et al. (2003). "An Initial Survey of White Dwarfs in the Sloan Digital Sky Survey". The Astronomical Journal 126 (2): 1023. doi:10.1086/376842. Bibcode: 2003AJ....126.1023H.
- ↑ Adelman-Mccarthy, J. K. (2011). "VizieR Online Data Catalog: The SDSS Photometric Catalog, Release 8 (Adelman-McCarthy+, 2011)". VizieR On-line Data Catalog. Bibcode: 2011yCat.2306....0A.
- ↑ 5.0 5.1 Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
- ↑ Brown, Warren R. (2006). "Hypervelocity Stars. I. The Spectroscopic Survey". The Astrophysical Journal 647 (1): 303–311. doi:10.1086/505165. Bibcode: 2006ApJ...647..303B.
- ↑ 7.0 7.1 7.2 7.3 Przybilla, N.; Nieva, M. F.; Tillich, A.; Heber, U.; Butler, K.; Brown, W. R. (2008). "HVS 7: A chemically peculiar hyper-velocity star". Astronomy & Astrophysics 488 (2): L51–L54. doi:10.1051/0004-6361:200810455. Bibcode: 2008A&A...488L..51P. "Such a surface abundance pattern is caused by atomic diffusion in a possibly magnetically stabilised, non-convective atmosphere. Hence all chemical information on the star’s place of birth and its evolution has been washed out. High precision astrometry is the only means to validate a GC origin for HVS 7.".
- ↑ 8.0 8.1 Brown, Warren R.; Geller, Margaret J.; Kenyon, Scott J.; Kurtz, Michael J. (2006). "Hypervelocity Stars. I. The Spectroscopic Survey". The Astrophysical Journal 647 (1): 303–311. doi:10.1086/505165. Bibcode: 2006ApJ...647..303B. "Here we report the two most recently discovered HVSs: SDSS J110557.45+093439.5 and possibly SDSS J113312.12+010824, traveling with Galactic rest-frame velocities at least +508+/-12 and +418+/-10 km s-1, respectively.".
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