Iota Horologii

Coordinates: Sky map 02h 42m 31.65s, −50° 48′ 12.29″
Source: Wikipedia, the free encyclopedia.

Iota Horologii
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Horologium
Right ascension 02h 42m 33.4665s[1]
Declination −50° 48′ 01.0562″[1]
Apparent magnitude (V) +5.40[citation needed]
Characteristics
Spectral type G0Vp[2]
B−V color index 0.57[citation needed]
Variable type none
Distance
56.61 ± 0.04 ly
(17.36 ± 0.01 pc)
Absolute magnitude (MV)+4.23[4]
Details
Gyr
HR 810, 2MASS J02423346-5048008[8]
Database references
SIMBADdata

Iota Horologii,

yellow dwarf (it has previously been classified as G3 and a subgiant [IV]). It has a mass and radius larger than the Sun
, and is about 50% more luminous.

In 1999, a planet of the star was discovered.

dust disc was announced around the star, but this was later determined to be an instrumental artifact.[10]

Distance and visibility

Since Iota Horologii is in the minor constellation of Horologium and is quite dim in the sky, it has not been given a traditional name. It lies roughly between the stars Eta Horologii and R Horologii (though it is not close to them in real space).

Location of Iota (ι) Horologii (circled)
Location of Iota (ι) Horologii (circled)

In its current position, Iota Horologii is closest to the star

yellow dwarf), approximately 57 light-years away, and Epsilon Reticuli (an orange subgiant), approximately 59 light-years away. Other star systems close to Iota Horologii include Nu Phoenicis and Zeta Reticuli.[2]

Properties

Hyades cluster (~625 million years ago) but must have slowly drifted away, being presently more than 130 light-years away from its original birthplace. The metallicity of the star matches the abundances found in the Hyades, indicating that the metals (elements heavier than helium) in the atmosphere were not acquired because it engulfed planetary material.[5]

Measurements of magnetic activity with the 1.5 m telescope at

magnetic activity cycle which, as of 2010, is the shortest cycle measured so far for a solar like star. The sun by comparison has an 11-year magnetic activity cycle. There may be a second, longer cycle which modulates the 1.6 year cycle.[11]

Planetary system

Iota Horologii b is believed to be Jupiter-sized.[9] The planet's discovery was the result of a survey of forty stars that began in November 1992.[12]

Stability analysis reveals that the orbits of Earth-sized planets located in the planet's

trojan points would be stable for long periods of time.[13]

Based on residuals in the radial velocity curve, a planet in an

eccentric orbit with a period of approximately 600 days was proposed, but this was not confirmed and it seems likely that the effect was due to activity on Iota Horologii itself.[12]

An

Gaia DR3.[14]

The Iota Horologii planetary system[15][14]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b 6.2±0.5 MJ 0.96 ± 0.05 307.2 ± 0.3 0.18 ± 0.03 87±6° —

See also

References

  1. ^
    doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR
    .
  2. ^ a b c "Iota Horologii". SolStation. Retrieved May 28, 2008.
  3. ^
    S2CID 244398875
    . Gaia DR3 record for this source at VizieR.
  4. S2CID 119257644
    .
  5. ^
    doi:10.1051/0004-6361:20079342
    .
  6. ^
    doi:10.1111/j.1365-2966.2010.16575.x
    .
  7. ^
    S2CID 119452853
    .
  8. ^ "Iota Horologii". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved August 15, 2020.
  9. ^ a b "Extrasolar Giant Planet in Earth-like Orbit" (Press release). Garching, Germany: European Southern Observatory. July 29, 1999. Retrieved December 29, 2012.
  10. ^ "Retracted in August 2001: ADONIS Discovers Dust Disk around a Star with a Planet" (Press release). Garching, Germany: European Southern Observatory. October 13, 2000. Retrieved December 30, 2012.
  11. doi:10.1088/2041-8205/723/2/L213
    .
  12. ^
    Bibcode:2000A&A...353L..33K. Archived from the original
    on July 25, 2011. Retrieved October 20, 2008.
  13. doi:10.1051/0004-6361:20077994
    .
  14. ^
    arXiv:2206.05595 [astro-ph.SR
    ].
  15. doi:10.1051/0004-6361/201116551
    .

External links


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