HD 114613

Last updated
HD 114613
Centaurus constellation map.svg
Red circle.svg
Location of HD 114613 (circled)
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Centaurus
Right ascension 13h 12m 03.18430s [1]
Declination −37° 48′ 10.8799″ [1]
Apparent magnitude  (V)4.852 ± 0.011 [2]
Characteristics
Spectral type G4 IV [3]
B−V color index 0.659 ± 0.020 [2]
Astrometry
Radial velocity (Rv)−13.03±0.13 [1]  km/s
Proper motion (μ)RA: −382.409  mas/yr [1]
Dec.: −46.147  mas/yr [1]
Parallax (π)48.8691 ± 0.1058  mas [1]
Distance 66.7 ± 0.1  ly
(20.46 ± 0.04  pc)
Absolute magnitude  (MV)3.29 [4]
Details
Mass 1.25±0.03 [5]   M☉
Radius 2.01±0.06 [5]   R☉
Luminosity 4.057±0.014 [6]   L☉
Surface gravity (log g)3.97±0.02 [6]   cgs
Temperature 5,729±17 [6]   K
Metallicity [Fe/H]0.19±0.01 [6]   dex
Rotation 34.1±3.5  d [7]
Rotational velocity (v sin i)2.4±0.5 [8]  km/s
Age 5.20±0.24 [5]   Gyr
Other designations
CD−37°8437, FK5  3051, GJ  501.2, HD  114613, HIP  64408, HR  4979, SAO  204227
Database references
SIMBAD data

HD 114613 (Gliese 501.2) is a fifth magnitude yellow subgiant star that lies 66.7 light-years (20.5 parsecs ) away in the constellation of Centaurus.

Contents

Stellar characteristics

The position of HD 114613 on the Hertzsprung-Russell diagram. The star lies significantly above the main sequence. HRDiagram.png
The position of HD 114613 on the Hertzsprung-Russell diagram. The star lies significantly above the main sequence.
Chess tile xg.svg

HD 114613 lies about two degrees south-east of Iota Centauri, towards the middle of Centaurus. Though it is fairly easily observable with the naked eye, the star does not have a Bayer or Flamsteed designation as the constellation of Centaurus contains many brighter stars.

The B-V colour and spectroscopic temperature of HD 114613 correspond with its spectral type of G4. This means that the star is only slightly cooler than the Sun, and has the yellow hue typical of G-type stars. On the Hertzsprung-Russell diagram (left) the star lies significantly above the main sequence, and is close to the subgiant branch; this means that HD 114613 has depleted the hydrogen in its core through nuclear fusion, and is increasing in radius while decreasing in temperature as it moves towards the giant branch.

As HD 114613 is ending hydrogen fusion, the star must be fairly old. When combined with a spectroscopically-derived mass of 1.25 ± 0.03 M☉ and a surface gravity of log 3.95 ± 0.03 g the implied age of the star is 5.20 ± 0.24 billion years, [5] making it slightly older than the Sun. Though stellar metallicities typically decrease with increasing stellar age, within the age range of the thin disk a wide range of metallicities are common; HD 114613's high iron abundance of 0.19 ± 0.01 dex (155 ± 4% of the solar abundance) is therefore not unusual. The rate of giant planet occurrence for Fe/H = 0.2 dex stars is about 15%, [9] which makes it fairly unsurprising that the star could host a giant planet.

HD 114613 has a magnetic cycle with a period of 897 ± 61 days, about four-and-a-half times shorter than the Solar magnetic cycle and one of the shortest magnetic cycles known. [7]

Planet searches

Being bright and solar-type, HD 114613 is an attractive target for radial velocity (RV)-based planet searches.

HD 114613 was one of the 37 targets of the first RV-based planet search in the southern hemisphere, the ESO-CES survey that spanned between 1992 and 1998. [10] This survey did not detect any companion with several Jovian masses out to a few AU. An extension of this survey to the HARPS spectrograph provides further constraint, suggesting that there are no Jupiter-mass companions out to about 5 AU. [11]

HD 114613 is included in the samples of the ESO-CORALIE [9] and AAT-UCLES [12] planet searches that both began in 1998. Seemingly finding the star to be RV-stable and suitable for higher precision, HD 114613 was included in a subset of the CORALIE sample that became the sample of the ESO-HARPS high precision planet search that began in 2004, [6] while the star was elevated in importance in the AAT sample in 2005. [13] [14] Though apparently not included in its main sample, HD 114613 is included in the sample of the Keck-HIRES Eta-Earth low-mass planet search that also began in 2004. [15]

In Wittenmyer et al. 2012, [16] HD 114613 is indicated to be a low-mass planet host. Though this references a Tuomi et al. 2012 (Tuomi, M., et al. 2012, MNRAS, submitted), no such paper was published that year. More recently, in a Tuomi et al. 2013, [17] Tau Ceti is noted to have a similar activity index distribution to HD 114613. Again, a Tuomi et al. 2012 is referenced, though somewhat more completely (Tuomi, M., Jones, H. R. A., Jenkins, J. S., et al. 2012, MNRAS, submitted). No paper announcing HD 114613 as a low-mass planet host has been published as of 2014.

However, that does not mean the star is not a planet host. Wittenmyer et al. (2014) found HD 114613 to show a moderate-amplitude variation in its radial velocity with a period of 10.5 years, indicative of a long-period companion. [18] The radial velocity semi-amplitude of 5.5 m/s translates to a planet with a minimum mass about half a Jupiter mass. The planet has an intermediate orbital eccentricity of 0.25, which means that it can be somewhat loosely considered a Jupiter analogue.

A study in 2023 did not detect this radial velocity signal, but instead detected a signal with a longer period of about 18 years, which shows indications of originating from a long-period magnetic activity cycle. This suggests that the previously detected signal is not planetary, but is related to stellar activity. [19] : 28  [19] : 44 

Related Research Articles

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References

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  2. 1 2 Høg, E.; et al. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: 27–30. Bibcode:2000A&A...355L..27H. doi:10.1888/0333750888/2862. ISBN   0333750888.
  3. ↑ Gray, R. O.; Corbally, C. J.; Garrison, R. F.; McFadden, M. T.; Bubar, E. J.; McGahee, C. E.; O'Donoghue, A. A.; Knox, E. R. (2006). "Contributions to the Nearby Stars (NStars) Project: Spectroscopy of Stars Earlier than M0 within 40 pc-The Southern Sample". The Astronomical Journal. 132 (1): 161–170. arXiv: astro-ph/0603770 . Bibcode:2006AJ....132..161G. doi:10.1086/504637. S2CID   119476992.
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  8. ↑ Valenti, J. A.; et al. (2005). "Spectroscopic Properties of Cool Stars (SPOCS). I. 1040 F, G, and K Dwarfs from Keck, Lick, and AAT Planet Search Programs". The Astrophysical Journal Supplement Series. 159 (1): 141–166. Bibcode:2005ApJS..159..141V. doi: 10.1086/430500 .
  9. 1 2 Mortier, A.; et al. (2013). "On the functional form of the metallicity-giant planet correlation". Astronomy & Astrophysics. 551: A112. arXiv: 1302.1851 . Bibcode:2013A&A...551A.112M. doi:10.1051/0004-6361/201220707. S2CID   56350455.
  10. ↑ Endl, M.; et al. (2002). "The planet search program at the ESO Coudé Echelle spectrometer. III. The complete Long Camera survey results". Astronomy & Astrophysics. 392 (2): 671–690. arXiv: astro-ph/0207512 . Bibcode:2002A&A...392..671E. doi:10.1051/0004-6361:20020937. S2CID   17393347.
  11. ↑ Zechmeister, M.; et al. (2013). "The planet search programme at the ESO CES and HARPS. IV. The search for Jupiter analogues around solar-like stars". Astronomy & Astrophysics. 592: A78. arXiv: 1211.7263 . Bibcode:2013A&A...552A..78Z. doi:10.1051/0004-6361/201116551. S2CID   53694238.
  12. ↑ Jones, Hugh R. A.; et al. (2002). "Extrasolar planets around HD 196050, HD 216437 and HD 160691". Monthly Notices of the Royal Astronomical Society . 337 (4): 1170–1178. arXiv: astro-ph/0206216 . Bibcode:2002MNRAS.337.1170J. doi: 10.1046/j.1365-8711.2002.05787.x . S2CID   119520409.
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  14. ↑ Wittenmyer, Robert A.; et al. (2011). "The Frequency of Low-mass Exoplanets. III. Toward η🜨 at Short Periods". The Astrophysical Journal. 738 (1): 81. arXiv: 1103.4186 . Bibcode:2011ApJ...738...81W. doi:10.1088/0004-637X/738/1/81. S2CID   19007954.
  15. ↑ Howard, Andrew A.; et al. (2010). "The Occurrence and Mass Distribution of Close-in Super-Earths, Neptunes, and Jupiters". Science. 330 (6004): 653–655. arXiv: 1011.0143 . Bibcode:2010Sci...330..653H. doi:10.1126/science.1194854. PMID   21030652. S2CID   34792507.
  16. ↑ Wittenmyer, Robert A.; et al. (2012). "The Anglo-Australian Planet Search. XXII. Two New Multi-planet Systems". The Astrophysical Journal. 753 (2): 169. arXiv: 1205.2765 . Bibcode:2012ApJ...753..169W. doi:10.1088/0004-637X/753/2/169. S2CID   2941264.
  17. ↑ Tuomi, M.; et al. (2013). "Signals embedded in the radial velocity noise. Periodic variations in the τ Ceti velocities". Astronomy & Astrophysics. 551: A79. arXiv: 1212.4277 . Bibcode:2013A&A...551A..79T. doi:10.1051/0004-6361/201220509. S2CID   2390534.
  18. ↑ Wittenmyer, Robert A.; et al. (2014). "The Anglo-Australian Planet Search. XXIII. Two New Jupiter Analogs". The Astrophysical Journal. 783 (2): 103. arXiv: 1401.5525 . Bibcode:2014ApJ...783..103W. doi:10.1088/0004-637X/783/2/103. S2CID   14082923.
  19. 1 2 Laliotis, Katherine; Burt, Jennifer A.; et al. (February 2023). "Doppler Constraints on Planetary Companions to Nearby Sun-like Stars: An Archival Radial Velocity Survey of Southern Targets for Proposed NASA Direct Imaging Missions". The Astronomical Journal . 165 (4): 176. arXiv: 2302.10310 . Bibcode:2023AJ....165..176L. doi: 10.3847/1538-3881/acc067 .
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