|Extrasolar planet||List of extrasolar planets|
| Parent star
<td style="text-align: center">(α)</td>
<td>02h 42m 33.466s</td></tr><tr>
<td style="text-align: center">(δ)</td>
<td>−50° 48′ 01.06″</td></tr><tr>
<td style="text-align: center">(mV)</td>
<td>5.4</td></tr><tr><td colspan="2">Distance</td><td>56.0 ± 0.2 ly
| Orbital elements
<tr><td>Semimajor axis</td><td style="text-align: center">(a)</td>
| Discovery information
<tr> <td colspan="2">Discovery date</td> <td>29 July 1999</td></tr><tr> <td colspan="2">Discoverer(s)</td> <td>Kürster et al.</td></tr><tr> <td colspan="2">Discovery method</td> <td>Doppler spectroscopy</td></tr><tr> <td colspan="2">Discovery site</td> <td>La Silla Observatory</td></tr><tr> <td colspan="2">Discovery status</td> <td>Published</td></tr>
<tr style="background-color: #A0B0FF;"><td align=center colspan=3>Database references</td></tr><tr valign=baseline><td colspan=2>Extrasolar Planets
Iota Horologii b (ι Hor b / ι Horologii b), often catalogued HR 810 b, is an extrasolar planet approximately 56 light-years away in the constellation of Horologium (the Pendulum Clock). Iota Horologii b has a minimum mass 1.94 times that of Jupiter, however preliminary astrometric measurements suggest that the object may be around 24 Jupiter masses and would therefore be a brown dwarf.
Detection and discovery Edit
The discovery of Iota Horologii b was the result of a long-term survey of forty solar twin stars that was begun in November 1992. The planet represents the first discovery of an extrasolar planet with a European Southern Observatory instrument, with the data found at the La Silla Observatory in Chile.
The Keplerian signal found the planet to have an orbital period of 320.1 days, indicative of an orbiting planet with minimum mass of 2.26 Jupiter masses. Iota Horologii b was announced in the summer of 1999 as the first planet found by a team of planet hunters led by Martin Kürster.
The measurements of Iota Horologii show that the planet orbits the star approximately every 320 days. From this period, the known mass of the central star (1.03 solar masses) and the amplitude of the velocity changes, a mass of at least 2.26 times that of planet Jupiter is deduced for the planet.
It revolves around the host star in a somewhat elongated orbit. If it were located in our own solar system, this orbit would stretch from just outside the orbit of Venus (at 117 million km or 0.78 astronomical unit [AU] from the Sun) to just outside the orbit of the Earth (at 162 million km or 1.08 AU). Because the planet is at least 720 times more massive than the Earth, it is predicted that Iota Horologii b is more similar to planet Jupiter.
In recent astrometric analysis of Iota Horologii b suggests that planet b may have as much as 24 times the mass of Jupiter with an inclination of 5.5 degrees from Earth's line of sight. With this calculations, Iota Horologii b may actually be an extremely dim brown dwarf and a substellar companion of Iota Horologii. However these measurements were later proved useful only for upper limits of inclination.
See also Edit
- ↑ 1.0 1.1 1.2 1.3 (2007). Validation of the new Hipparcos reduction. Astronomy and Astrophysics 474 (2): 653–664. Vizier catalog entry
- ↑ 2.0 2.1 Script error
- ↑ 3.0 3.1 (2000). An extrasolar giant planet in an Earth-like orbit. Precise radial velocities of the young star iota Horologii = HR 810. Astronomy and Astrophysics 353 (3): L33–L36.
- ↑ (2001). The CORALIE survey for southern extrasolar planets V. 3 new extrasolar planets. Astronomy and Astrophysics 375 (1): 205–218.
- ↑ Retracted in August 2001: ADONIS Discovers Dust Disk around a Star with a Planet. European Southern Observatory (2000-10-13). Retrieved 2011-12-21.
- ↑ Pourbaix, D. and Arenou, F. (2001). Screening the Hipparcos-based astrometric orbits of sub-stellar objects. Astronomy and Astrophysics 372 (3): 935–944.
- Extrasolar Giant Planet in Earth-like Orbit. European Southern Observatory. Retrieved 2008-06-12.
- Iota Horologii. SolStation. Retrieved 2008-06-12.
- The Planet Around HD17051. California & Carnegie Planet Search Team (2003-05-04). Retrieved 2008-06-12.