109 Piscium

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109 Piscium
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Pisces
Right ascension 01h 44m 55.8251s [1]
Declination +20° 04′ 59.3363″ [1]
Apparent magnitude  (V)6.27 [2]
Characteristics
Spectral type G3 Va [3]
U−B color index 0.23[ citation needed ]
B−V color index 0.720±0.009 [2]
Variable type none
Astrometry
Radial velocity (Rv)−45.53±0.09 [4]  km/s
Proper motion (μ)RA: −42.979±0.069 [1]   mas/yr
Dec.: −104.889±0.068 [1]   mas/yr
Parallax (π)30.1639 ± 0.0400  mas [1]
Distance 108.1 ± 0.1  ly
(33.15 ± 0.04  pc)
Absolute magnitude  (MV)3.73 [5]
Details
Mass 1.11±0.03 [6]   M☉
Radius 1.9155±0.0521 [7]   R☉
Luminosity 2.8888±0.0833 [7]   L☉
Temperature 5,600±75 [8]   K
Metallicity [Fe/H]0.15±0.04 [4]   dex
Rotation 32.6±1.6 d [9]
Rotational velocity (v sin i)1.3 [5]  km/s
Age 6.75±0.71 [6]   Gyr
Other designations
BD+19° 282, GJ  72, HD  10697, HIP  8159, HR  508 [8]
Database references
SIMBAD data

109 Piscium is a yellow hued G-type main-sequence star located about 108 light-years away in the zodiac constellation of Pisces. It is near the lower limit of visibility to the naked eye with an apparent visual magnitude of 6.27. [2] The star is moving closer to the Earth with a heliocentric radial velocity of −45.5 km/s. [4] It has one known exoplanet. [10]

Contents

With a stellar classification of G3 Va, [3] this is a Sun-like star with a similar mass [6] but a 91% [7] larger radius. (Cowley and Bidelman (1979) had this classified as a subgiant star that is leaving the main sequence. [11] ) It is 6.75 [6]  billion years old with a higher abundance of iron [4] and a low projected rotational velocity of 1.3 km/s. [5] The star is radiating 2.9 [7] times the Sun's luminosity from its photosphere at an effective temperature of 5,442  K . [7]

Planetary system

On 1 November 1999 the discovery of an extrasolar planet orbiting this star was announced. [10] The planet has a minimum mass of about 6 times that of Jupiter and takes just under three years to orbit its parent star. [12] It orbits within the habitable zone. [10]

The star rotates at an inclination of 69+21
−26 degrees relative to Earth. [9] It is probable that this planet shares that inclination. [13] [14] In 2022, the inclination and true mass of 109 Piscium b were measured via astrometry. The inclination estimate is consistent with that of the stellar rotation. [15]

The 109 Piscium planetary system [16] [15]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
b 5.743+1.011
−0.289  MJ 		2.051+0.079
−0.087		2.944±0.0020.104+0.009
−0.008		86.116+19.957
−20.530 ° 		—

In the 1983 Star Trek novel The Wounded Sky by Diane Duane, the USS Enterprise intentionally causes 109 Piscium to go supernova by engaging its warp drive too close to the star, in order to destroy a group of pursuing Klingon vessels. Mr. Spock informs the "Interstellar Astronomical Union" of the change in status of the star, and Captain Kirk experiences an uneasy sense that he may "get in trouble with Starfleet" over this arguably rash course of action.

See also

Related Research Articles

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<span class="mw-page-title-main">109 Piscium b</span> Long-period gas giant orbiting 109 Piscium

109 Piscium b is a long-period extrasolar planet discovered in orbit around 109 Piscium. It is about 5.74 times the mass of Jupiter and is likely to be a gas giant. As is common for long-period planets discovered around other stars, it has an orbital eccentricity greater than that of Jupiter.

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References

  1. 1 2 3 4 5 Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics . 616. A1. arXiv: 1804.09365 . Bibcode: 2018A&A...616A...1G . doi: 10.1051/0004-6361/201833051 . Gaia DR2 record for this source at VizieR.
  2. 1 2 3 Anderson, E.; Francis, Ch. (2012), "XHIP: An extended hipparcos compilation", Astronomy Letters, 38 (5): 331, arXiv: 1108.4971 , Bibcode:2012AstL...38..331A, doi:10.1134/S1063773712050015, S2CID   119257644.
  3. 1 2 Keenan, P.; McNeil, R. (October 1989), "The Perkins catalog of revised MK types for the cooler stars", Astrophysical Journal Supplement Series, 71: 245–266, Bibcode:1989ApJS...71..245K, doi:10.1086/191373.
  4. 1 2 3 4 Jofré, E.; et al. (2015), "Stellar parameters and chemical abundances of 223 evolved stars with and without planets", Astronomy & Astrophysics, 574: A50, arXiv: 1410.6422 , Bibcode:2015A&A...574A..50J, doi:10.1051/0004-6361/201424474, S2CID   53666931.
  5. 1 2 3 Pizzolato, N.; Maggio, A.; Sciortino, S. (September 2000), "Evolution of X-ray activity of 1-3 Msun late-type stars in early post-main-sequence phases", Astronomy and Astrophysics, 361: 614–628, Bibcode:2000A&A...361..614P.
  6. 1 2 3 4 Ghezzi, L.; et al. (December 2010), "Metallicities of Planet-hosting Stars: A Sample of Giants and Subgiants", The Astrophysical Journal, 725 (1): 721–733, arXiv: 1008.3539 , Bibcode:2010ApJ...725..721G, doi:10.1088/0004-637X/725/1/721, S2CID   119206634.
  7. 1 2 3 4 5 Boyajian, Tabetha S.; et al. (2013). "Stellar Diameters and Temperatures. III. Main-Sequence A, F, G, and K Stars: Additional High-Precision Measurements and Empirical Relations". The Astrophysical Journal. 771 (1). 40. arXiv: 1306.2974 . Bibcode:2013ApJ...771...40B. doi: 10.1088/0004-637X/771/1/40 .
  8. 1 2 "109 Psc -- High proper-motion Star". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 20 December 2017.
  9. 1 2 Simpson, E. K.; et al. (November 2010), "Rotation periods of exoplanet host stars", Monthly Notices of the Royal Astronomical Society , 408 (3): 1666–1679, arXiv: 1006.4121 , Bibcode:2010MNRAS.408.1666S, doi:10.1111/j.1365-2966.2010.17230.x, S2CID   6708869. as "HD 10697"
  10. 1 2 3 "Astronomers discover six new planets orbiting nearby stars" (Press release). Kamuela, Hawaii: W. M. Keck Observatory. 1 November 1999. Retrieved 19 December 2017.
  11. ↑ Cowley, A. P.; Bidelman, W. P. (February 1979), "MK spectral types for some F and G stars", Publications of the Astronomical Society of the Pacific, 91: 83–86, Bibcode:1979PASP...91...83C, doi:10.1086/130446
  12. ↑ Vogt, Steven S.; et al. (2000). "Six New Planets from the Keck Precision Velocity Survey". The Astrophysical Journal. 536 (2): 902–914. arXiv: astro-ph/9911506 . Bibcode: 2000ApJ...536..902V . doi: 10.1086/308981 .
  13. ↑ "hd_10697_b". Extrasolar Planet Encyclopaedia. 26 November 1995. Retrieved 12 November 2012.
  14. ↑ Sanchis-Ojeda, Roberto; Winn, Josh N.; Fabrycky, Daniel C. (2012). "Starspots and spin-orbit alignment for Kepler cool host stars". Astronomische Nachrichten. 334 (1–2): 180–183. arXiv: 1211.2002 . Bibcode:2013AN....334..180S. doi:10.1002/asna.201211765. S2CID   38743202.
  15. 1 2 Feng, Fabo; Butler, R. Paul; et al. (August 2022). "3D Selection of 167 Substellar Companions to Nearby Stars". The Astrophysical Journal Supplement Series . 262 (21): 21. arXiv: 2208.12720 . Bibcode:2022ApJS..262...21F. doi: 10.3847/1538-4365/ac7e57 . S2CID   251864022.
  16. ↑ Luhn, Jacob K.; et al. (2019). "Retired A Stars and Their Companions. VIII. 15 New Planetary Signals around Subgiants and Transit Parameters for California Planet Search Planets with Subgiant Hosts". The Astronomical Journal. 157 (4). 149. arXiv: 1811.03043 . Bibcode:2019AJ....157..149L. doi: 10.3847/1538-3881/aaf5d0 . S2CID   102486961.
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