„Zeta Leporis“ – Versionsunterschied
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| epoch = [[J2000.0]] |
| epoch = [[J2000.0]] |
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| constell = [[Lepus (constellation)|Lepus]] |
| constell = [[Lepus (constellation)|Lepus]] |
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| ra={{RA|05|46|57.341}}<ref name="SIMBAD-Gliese217.1"/> |
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| dec={{DEC|−14|49|19.02}} |
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|appmag_v=3.55<ref name="SIMBAD-Gliese217.1">{{cite web |
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|title=Gliese 217.1 |
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|publisher=SIMBAD Astronomical Database |
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|url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gliese+217.1 |
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|accessdate=2010-03-19}}</ref> |
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| mass = 2 |
| mass = 2<ref name="Bobylev:arXiv1003.2160"/> |
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| radius = 1.7 |
| radius = 1.7 |
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| luminosity = 15 |
| luminosity = 15 |
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== Stellar components == |
== Stellar components == |
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Zeta Leporis is a [[white main sequence star]] (not to be confused with a [[white dwarf]]) of the [[spectral type]] of "A2-3Vann". The star is though to have about two times the [[mass]] of the [[Sun]], along with 1.7 times the [[radius]], and 15 times the [[luminosity]]. The star appears to be a very young star, probably around 100 million years old, but could be anywhere between 50 and 500 million years old. The star was suggested to be a [[spectroscopic binary]] star. But because this secondary star was not confirmed, there is no data on the star. |
Zeta Leporis is a [[naked eye]] star with an [[apparent magnitude]] of 3.5.<ref name="SIMBAD-Gliese217.1"/> It is a [[white main sequence star]] (not to be confused with a [[white dwarf]]) of the [[spectral type]] of "A2-3Vann". The star is though to have about two times the [[mass]] of the [[Sun]], along with 1.7 times the [[radius]], and 15 times the [[luminosity]]. The star appears to be a very young star, probably around 100 million years old, but could be anywhere between 50 and 500 million years old. The star was suggested to be a [[spectroscopic binary]] star. But because this secondary star was not confirmed, there is no data on the star. |
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== Asteroid belt == |
== Asteroid belt == |
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== Solar encounter == |
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Bobylev's calculations from 2010 suggest that this star passed as close as 1.28 [[parsec]]s (4.17 [[light-year]]s) from the Sun about 861 thousand years ago.<ref name="Bobylev:arXiv1003.2160">{{cite journal |last=Bobylev |first=Vadim V. |authorlink= |year=2010 |month=March |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220-226 |doi=10.1134/S1063773710030060 |url=http://arxiv.org/abs/1003.2160 |accessdate= |quote= }} </ref> |
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== See also == |
== See also == |
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== References == |
== References == |
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{{reflist}} |
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* Cote, J., 1987, "B and A type stars with unexpectedly large colour excesses at IRAS wavelengths", ''Astronomy and Astrophysics'', vol. 181, no. 1. |
* Cote, J., 1987, "B and A type stars with unexpectedly large colour excesses at IRAS wavelengths", ''Astronomy and Astrophysics'', vol. 181, no. 1. |
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* Aumann, H. H.; Probst, R. G, 1991, "Search for Vega-like nearby stars with 12 micron excess", ''Astrophysical Journal'', vol. 368, Feb. 10. |
* Aumann, H. H.; Probst, R. G, 1991, "Search for Vega-like nearby stars with 12 micron excess", ''Astrophysical Journal'', vol. 368, Feb. 10. |
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Version vom 19. März 2010, 05:16 Uhr
Vorlage:Starbox begin Vorlage:Starbox observe Vorlage:Starbox character Vorlage:Starbox astrometry Vorlage:Starbox detail Vorlage:Starbox catalog Vorlage:Starbox reference Vorlage:Starbox end
Zeta Leporis (ζ Lep / ζ Leporis) white main sequence star approximately 70 light-years away in the constellation of Lepus. The star is suspected of being a spectroscopic binary star system, but this is yet to be confirmed. As of 2001, an asteroid belt was confirmed to orbit around the star.
Stellar components
Zeta Leporis is a naked eye star with an apparent magnitude of 3.5.[1] It is a white main sequence star (not to be confused with a white dwarf) of the spectral type of "A2-3Vann". The star is though to have about two times the mass of the Sun, along with 1.7 times the radius, and 15 times the luminosity. The star appears to be a very young star, probably around 100 million years old, but could be anywhere between 50 and 500 million years old. The star was suggested to be a spectroscopic binary star. But because this secondary star was not confirmed, there is no data on the star.
Asteroid belt
In 1983, based on radiation in the infrared portion of the electromagnetic spectrum, the Astronomical Satellite was used to identify dust orbiting this star. The region containing the dust was constricted to a radius of 12.2 Astronomical units, or just over twelve times the distance from the Earth to the Sun.
By 2001, the Long Wavelength Spectrometer at the Keck Observatory on Mauna Kea, Hawaii, was used more accurately constrain the radius of the dust. It was found to lie within a 5.4 AU radius. The temperature of the dust was estimated as about 340 K. Based on heating from the star, this could place the grains as close as 2.5 AU from Zeta Leporis.
It is now believed that the dust is coming from a massive asteroid belt in orbit around Zeta Leporis, making it the first extra-solar asteroid belt to be discovered. The estimated mass of the belt is about 200 times the total in our own asteroid belt, or 4 × 1023 kg. (For comparison, that is more than half the total mass of our Moon.) The belt's age is estimated to be 3 × 108 years.
Vorlage:PlanetboxOrbit begin Vorlage:PlanetboxOrbit disk Vorlage:PlanetboxOrbit end
Solar encounter
Bobylev's calculations from 2010 suggest that this star passed as close as 1.28 parsecs (4.17 light-years) from the Sun about 861 thousand years ago.[2]
See also
References
- Cote, J., 1987, "B and A type stars with unexpectedly large colour excesses at IRAS wavelengths", Astronomy and Astrophysics, vol. 181, no. 1.
- Aumann, H. H.; Probst, R. G, 1991, "Search for Vega-like nearby stars with 12 micron excess", Astrophysical Journal, vol. 368, Feb. 10.
- Chen, C. H.; Jura, M., 2001, "A Possible Massive Asteroid Belt around zeta Leporis", Astrophysical Journal, Volume 560, Issue 2.
- M. M. Moerchen, C. M. Telesco, C. Packham, T. J. J. Kehoe: Mid-infrared resolution of a 3 AU-radius debris disk around Zeta Leporis. In: Astrophysical Journal Letters. 2006 (arxiv.org [SUBSCRIPTION REQUIRED]).
External links
- Robert Roy Britt: Asteroid Belt Like Ours Spotted Around Another Star. In: SPACE.com. 4. Juni 2001, abgerufen am 26. Juni 2008.
- UCLA astronomers identify evidence of asteroid belt around nearby star: Findings indicate potential for planet or asteroid formation, 2001.
- Zeta Leporis. In: Extrasolar Visions. Abgerufen am 26. Juni 2008.
- Zeta Leporis Asteroid Belt. In: Extrasolar Visions. Abgerufen am 26. Juni 2008.
- Zeta Leporis. In: SolStation. Abgerufen am 26. Juni 2008.
- ↑ Referenzfehler: Ungültiges
<ref>-Tag; kein Text angegeben für Einzelnachweis mit dem Namen SIMBAD-Gliese217.1. - ↑ Vadim V. Bobylev: Searching for Stars Closely Encountering with the Solar System. In: Astronomy Letters. 36. Jahrgang, Nr. 3, März 2010, S. 220–226, doi:10.1134/S1063773710030060 (arxiv.org).