| absmag_v = +1.88[12]
}}{{Starbox detail
| mass = 1.46[13]
| radius = 1.5[14]
| luminosity = 14[15]
| temperature = {{val|9772|fmt=commas}}[16]
| gravity = 4.41[15]
| metal_fe = –0.76[4]
| rotational_velocity = 245[14]
| age_myr = {{val|231|+126|-181}}[16]
}}{{Starbox catalog
| names = ζ Lep, 14 Leporis, BD–14° 1232, FK5 219, GCTP 1326, Gl 217.1, HD 38678, HIP 27288, HR 1998, SAO 150801, Wolf 9190.[21]
}}{{Starbox reference
| Simbad = HD+38678
| ARICNS = 00464
}}{{Starbox end}}Zeta Leporis, Latinized from ζ Leporis, is a star approximately {{Convert|70.5|ly|pc|abbr=off|lk=on}} away in the southern constellation of Lepus. It has an apparent visual magnitude of 3.5,[3] which is bright enough to be seen with the naked eye. In 2001, an asteroid belt was confirmed to orbit the star.
Stellar components
Zeta Leporis has a stellar classification of A2 IV-V(n),[4] suggesting that it is in a transitional stage between an A-type main-sequence star and a subgiant. The (n) suffix indicates that the absorption lines in the star's spectrum appear nebulous because it is spinning rapidly, causing the lines to broaden because of the Doppler effect. The projected rotational velocity is 245 km/s,[14] giving a lower limit on the star's actual equatorial azimuthal velocity.
The star has about 1.46 times the mass of the Sun,[13] along with 1.5 times the radius,[14] and 14 times the luminosity.[15] The abundance of elements other than hydrogen and helium, what astronomers term the star's metallicity, is only 17% of the abundance in the Sun.[4] The star appears to be a very young, probably around 231 million years in age, but the margin of error spans 50–347 million years old.[16]
Asteroid belt
{{Multiple image|direction=vertical|align=left|image1=Asteroidbelt 01.jpg|image2=Asteroidbelt 02.jpg|width=150|caption2=A size comparison of the asteroid belt of the Solar System (top) and the Zeta Leporis asteroid belt (bottom).}}In 1983, based on radiation in the infrared portion of the electromagnetic spectrum, the InfraRed Astronomical Satellite was used to identify dust orbiting this star. This debris disk is constrained to a diameter of 12.2 AU.[30]
By 2001, the Long Wavelength Spectrometer at the Keck Observatory on Mauna Kea, Hawaii, was used more accurately to constrain the radius of the dust. It was found to lie within a 5.4 AU radius.[30] The temperature of the dust was estimated as about 340 K.{{Citation needed|date=May 2011}} Based on heating from the star, this could place the grains as close as 2.5 AU from Zeta Leporis.[30]
It is now believed{{By whom|date=September 2010}} 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 mass in the Solar System's asteroid belt, or {{val|4|e=23|u=kg}}. For comparison, this is more than half the total mass of the Moon. Astronomers Christine Chen and professor Michael Jura found that the dust contained within this belt should have fallen into the star within {{val|20000}} years, a time period much shorter than Zeta Leporis's estimated age, suggesting that some mechanism must be replenishing the belt.[30] The belt's age is estimated to be {{val|3|e=8}} years.{{Citation needed|date=September 2010}}
{{OrbitboxPlanet begin}}{{OrbitboxPlanet disk
| disk = Asteroid belt
| periapsis = 2.5
| apoapsis = 6.1
}}{{Orbitbox 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 861,000 years ago.[1] García-Sánchez 2001 suggested that the star passed 1.64 parsecs (5.34 light-years) from the Sun about 1 million years ago.[7]
See also
- Delta Trianguli
- HD 69830
- Vega
References
1. ^1 {{Cite journal|last=Bobylev |first=Vadim V. |date=March 2010 |title=Searching for Stars Closely Encountering with the Solar System |journal=Astronomy Letters |volume=36 |issue=3 |pages=220–226 |doi=10.1134/S1063773710030060 |arxiv=1003.2160 |bibcode=2010AstL...36..220B}}
2. ^1 {{citation | title=XHIP: An extended hipparcos compilation | last1=Anderson | first1=E. | last2=Francis | first2=Ch. | journal=Astronomy Letters | volume=38 | issue=5 | pages=331 | year=2012 | bibcode=2012AstL...38..331A | doi=10.1134/S1063773712050015 | arxiv=1108.4971 | postscript=. }}
3. ^1 2 3 4 {{citation | display-authors=1 | last1=Akeson | first1=R. L. | last2=Ciardi | first2=D. R. | last3=Millan-Gabet | first3=R. | last4=Merand | first4=A. | last5=Folco | first5=E. Di | last6=Monnier | first6=J. D. | last7=Beichman | first7=C. A. | last8=Absil | first8=O. | last9=Aufdenberg | first9=J. | title=Dust in the inner regions of debris disks around a stars | journal=The Astrophysical Journal | volume=691 | issue=2 | pages=1896–1908 |date=February 2009 | doi=10.1088/0004-637X/691/2/1896 | bibcode=2009ApJ...691.1896A |arxiv = 0810.3701 }}
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6. ^1 {{Cite web | title=Gliese 217.1 | work=SIMBAD Astronomical Object Database | publisher=Centre de Données astronomiques de Strasbourg | url=http://simbad.u-strasbg.fr/simbad/sim-id?Ident=Gliese+217.1 | accessdate=2010-03-19 }}
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