107 Piscium

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107 Piscium
Observation data
Epoch J2000.0        Equinox J2000.0 (ICRS)
Constellation Pisces
Right ascension 01h 42m 29.76349s [1]
Declination +20° 16′ 06.6602″ [1]
Apparent magnitude  (V)5.14 to 5.26 [2]
Characteristics
Spectral type K1V [3]
U−B color index +0.49 [4]
B−V color index +0.84 [4]
V−R color index 0.5 [5]
R−I color index +0.43 [4]
Variable type Constant [6]
Astrometry
Radial velocity (Rv)−33.619±0.0013 [7]  km/s
Proper motion (μ)RA: −301.592 [1]   mas/yr
Dec.: −674.505 [1]   mas/yr
Parallax (π)131.4903 ± 0.1515  mas [1]
Distance 24.80 ± 0.03  ly
(7.605 ± 0.009  pc)
Absolute magnitude  (MV)5.87 [8]
Details [9]
Mass 0.86  M☉
Radius 0.82±0.03  R☉
Luminosity (bolometric)0.46 [8]   L☉
Surface gravity (log g)4.57±0.10  cgs
Temperature 5,172±80  K
Metallicity [Fe/H]−0.01±0.07  dex
Rotation 35.0 days [10]
Rotational velocity (v sin i)2.0±1.0 km/s
Age 6.3 [11]   Gyr
Other designations
107 Psc, BD+19°279, GC  2080, HD  10476, HIP  7981, HR  493, SAO  74883, PPM  91014, CCDM J01425+2016A, WDS 01425+2016A, LFT  153, LHS  1287, LTT  10596, NLTT  5685 [5] [12]
Database references
SIMBAD data

107 Piscium is a single [13] star in the constellation of Pisces. 107 Piscium is the star's Flamsteed designation. John Flamsteed numbered the stars of Pisces from 1 to 113, publishing his Catalogus Britannicus in 1725. He accidentally numbered 107 Piscium twice, as he also allocated it the designation of 2 Arietis. [14] This star is faintly visible to the naked eye with an apparent visual magnitude that has been measured varying between 5.14 and 5.26. [2] However, that finding of variation was not confirmed by subsequent observations and is most likely spurious data. [6] It is located at a distance of about 24.8  light years away from the Sun. [1] 107 Piscium is drifting closer to the Sun with a radial velocity of −33.6, [7] and is predicted to come as close as 15.4 light-years in around 135,800 years. [15]

This object is a K-type main-sequence star with a stellar classification of K1V, [3] indicating it is generating energy from core hydrogen fusion. It is somewhat older than the Sun—approximately 6 billion years old. [11] The star has 86% of the mass and 82% of the radius of the Sun, [9] but shines with only 46% of the Sun's luminosity. [8] The effective temperature of the star is 5,172  K . [9] It is rotating slowly with a period of 35.0 d. [10] The abundance of elements other than hydrogen and helium—the star's metallicity—is slightly lower than that of the Sun. [16] The level of chromospheric activity is similar to the Sun, and it shows a simple cycle of variation. [17] [18]

107 Piscium has been examined for the presence of an infrared excess caused by exozodiacal dust, but none was detected. [19] The habitable zone for this star, defined as the locations where liquid water could be present on an Earth-like planet, is at a radius of 0.52–1.10  Astronomical Units (AU), where 1 AU is the average distance from the Earth to the Sun. [19]

In 1997, based on data collected during the Hipparcos mission, the star was categorized as an astrometric binary with a period of 0.576 years. However, this result has not been not confirmed. [20]

Related Research Articles

101 Piscium is a star in the zodiac constellation of Pisces, located around 1,400 light years away from the Sun. This appears as a dim, blue-white hued star near the lower limit of visibility to the naked eye at an apparent visual magnitude of 6.23. It is a suspected variable star with the designation NSV 559; 101 Piscium is the Flamsteed designation. The star is moving closer to the Earth with a heliocentric radial velocity of −10 km/s.

107 Aquarii is a double star in the equatorial constellation of Aquarius. 107 Aquarii is the Flamsteed designation, although it also bears the Bayer designation i2 Aquarii. The pair have an angular separation of 6.787 arcseconds. They have a combined apparent visual magnitude of +5.305, with individual magnitudes of 5.72 and 6.72. The annual parallax shift measured for the two components is 16.1 mas and 20.0 mas respectively, although with significant statistical margins of error and flags for potential unreliability of both values. This indicates the system may be at a distance of 160–200 light-years from Earth.

41 Aquarii is a double star in the equatorial constellation of Aquarius. 41 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, orange-hued point of light with a combined apparent visual magnitude of 5.354. The pair are located at a distance of around 239 light-years from the Sun based on parallax, but are drifting closer with a radial velocity of –25 km/s.

44 Aquarii is a single star located 336 light years away from the Sun in the equatorial constellation of Aquarius. 44 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.75. This body is moving away from the Earth with a heliocentric radial velocity of +7.4 km/s.

60 Aquarii is a star located 375 light years away from the Sun in the equatorial constellation of Aquarius. 60 Aquarii is its Flamsteed designation. It is visible to the naked eye as a dim, yellow-hued star with an apparent visual magnitude of 5.89. The star is moving closer to the Earth with a heliocentric radial velocity of –8 km/s.

HD 4628 is a main sequence star in the equatorial constellation of Pisces. It has a spectral classification of K2.5 V and an effective temperature of 5,055 K, giving it an orange-red hue with a slightly smaller mass and girth than the Sun. HD 4628 lies at a distance of approximately 24.3 light years from the Sun based on parallax. The apparent magnitude of 5.7 is just sufficient for this star to be viewed with the unaided eye. The star appears to be slightly older than the Sun—approximately 5.4 billion years in age. The surface activity is low and, based upon the detection of UV emission, it may have a relatively cool corona with a temperature of one million K.

72 Herculis is a single star in the northern constellation of Hercules. The Flamsteed designation for this star comes from the publication Historia Coelestis Britannica by John Flamsteed. It is the 72nd star in Flamsteed's list of stars in Hercules. This star is faintly visible to the naked eye with an apparent visual magnitude of 5.4. Parallax measurements show this star to be located at a distance of about 47 light years from the Sun. It is drifting closer with a radial velocity of −78.6 km/s, and is predicted to come to within 32.1 light-years in around 98,000 years.

HD 222582 is a multiple star system in the equatorial constellation of Aquarius. It is invisible to the naked eye with an apparent visual magnitude of 7.7, but can be viewed with binoculars or a small telescope. The system is located at a distance of 137 light years from the Sun based on parallax, and it is drifting further away with a radial velocity of +12 km/s. It is located close enough to the ecliptic that it is subject to lunar occultations.

HD 224635 and HD 224636 is a pair of stars comprising a binary star system in the constellation Andromeda. They are located approximately 94 light years away and they orbit each other every 717 years.

GJ 3379 is the nearest star in the Orion constellation, located at a distance of 17 light years from the Sun based on parallax. It is a single star with an apparent visual magnitude of +11.31 and an absolute magnitude of +12.71, therefore, the star is not visible with the naked eye. It is positioned in the upper left part of the Orion constellation, to the SSE of Betelgeuse. This star is drifting further away with a radial velocity of +30.0 kilometers per second. In the past, this star had a relatively close encounter with the Solar System. Some 161,000±6,000 years ago, it achieved a minimum distance of 4.08 ± 0.20 ly (1.25 ± 0.06 pc).

20 Camelopardalis is a solitary star in the circumpolar constellation Camelopardalis. It has an apparent magnitude of 7.45, making it readily visible in binoculars but not to the naked eye. Located about 880 light years away, it is approaching the Solar System with a radial velocity of −50.3 km/s. Due to its faintness, 20 Cam is one of the 220 Flamsteed stars without Bright Star Catalog designations.

Psi<sup>3</sup> Piscium Star in the constellation Pisces

Psi3 Piscium, which is Latinized from ψ3 Piscium, is a solitary, yellow-hued star in the zodiac constellation of Pisces. It is faintly visible to the naked eye, having an apparent visual magnitude of 5.562. Based upon an annual parallax shift of 7.5 mas as seen from Earth, it is located about 435 light years from the Sun. At that distance, the visual magnitude is diminished by an extinction factor of 0.33 due to interstellar dust. The star is drifting closer to the Sun with a radial velocity of −7 km/s.

16 Comae Berenices is a single star in the northern constellation of Coma Berenices. 16 Comae Berenices is the Flamsteed designation. It is a member of the Coma Star Cluster and is visible to the naked eye with an apparent visual magnitude of 4.96. Based upon an annual parallax shift of 11.7 mas, it is located about 279 light years away.

<span class="mw-page-title-main">Theta Sagittae</span> Double star in the constellation Sagitta

Theta Sagittae (θ Sagittae) is a double star in the northern constellation of Sagitta. With a combined apparent visual magnitude of +6, it is near the limit of stars that can be seen with the naked eye. According to the Bortle scale the star is visible in dark suburban/rural skies. Based upon an annual parallax shift of 22.15 mas as seen from Earth, it is located roughly 147 light years from the Sun.

58 Hydrae is a single star in the equatorial constellation of Hydra, located around 290 light years away from the Sun based on parallax. It has the Bayer designation E Hydrae; 58 Hydrae is the Flamsteed designation − a later designation of 6 Librae. It is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 4.42. This object is moving closer to the Earth with a heliocentric radial velocity of −9 km/s.

7 Piscium is a single star in the zodiac constellation of Pisces, located around 343 light-years away from the Sun. It has the Bayer designation b Piscium; 7 Piscium is the Flamsteed designation. This object is visible to the naked eye as a faint, orange-hued star with an apparent visual magnitude of 5.07. It is moving further from the Earth with a heliocentric radial velocity of 40 km/s.

26 Cygni is a single star in the northern constellation of Cygnus. It has the Bayer designation e Cygni, while 26 Cygni is the Flamsteed designation. This star is visible to the naked eye as a faint, yellow-hued point of light with an apparent visual magnitude of 5.12. It is located around 451 light-years (138 pc) distant from the Sun, based on parallax measurements. The radial velocity is close to negligible, being measured at −0.3 km/s.

10 Canum Venaticorum is the Flamsteed designation for an ordinary star in the northern constellation of Canes Venatici. It has an apparent visual magnitude of 5.95, which, according to the Bortle scale, can be faintly seen with the naked eye from suburban locations. Based upon an annual parallax shift of 0.057 arcseconds, this system is 57.26 light-years from Sun. It is drifting further away with a radial velocity of +80 km/s.

<span class="mw-page-title-main">Gliese 908</span> Star in the constellation Pisces

Gliese 908 is a red dwarf star, located in constellation Pisces at 19.3 light-years from Earth. It is a BY Draconis variable star with a variable star designation of BR Piscium. Its apparent magnitude varies between magnitude 8.93 and magnitude 9.03 as a result of starspots and varying chromospheric activity.

HD 44120 is a wide binary star system in the southern constellation of Pictor. Although visible to the naked eye, it is a challenge to view having an apparent visual magnitude of 6.44. The system is located at a distance of 118 light years from the Sun based on parallax, but it is drifting closer with a radial velocity of −2 km/s. It has an absolute magnitude of 3.57.

References

  1. 1 2 3 4 5 6 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 NSV 600, database entry, New Catalogue of Suspected Variable Stars, the improved version, Sternberg Astronomical Institute, Moscow, Russia. Accessed on line September 24, 2008.
  3. 1 2 Keenan, Philip C.; McNeil, Raymond C. (1989). "The Perkins catalog of revised MK types for the cooler stars". The Astrophysical Journal Supplement Series. 71: 245. Bibcode:1989ApJS...71..245K. doi:10.1086/191373.
  4. 1 2 3 HR 493, database entry, The Bright Star Catalogue, 5th Revised Ed. (Preliminary Version), D. Hoffleit and W. H. Warren, Jr., CDS ID V/50. Accessed on line September 24, 2008.
  5. 1 2 "107 Psc". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved September 24, 2008.
  6. 1 2 Lockwood, G. W.; et al. (August 1997). "The Photometric Variability of Sun-like Stars: Observations and Results, 1984-1995". The Astrophysical Journal. 485 (2): 789–811. Bibcode:1997ApJ...485..789L. doi: 10.1086/304453 .
  7. 1 2 Soubiran, C.; et al. (2018). "Gaia Data Release 2. The catalogue of radial velocity standard stars". Astronomy and Astrophysics. 616: A7. arXiv: 1804.09370 . Bibcode:2018A&A...616A...7S. doi:10.1051/0004-6361/201832795. S2CID   52952408.
  8. 1 2 3 HD 10476, catalog entry, Fundamental parameters and elemental abundances of 160 F-G-K stars based on OAO spectrum database, Y. Takeda, CDS ID J/PASJ/59/335; see also Publications of the Astronomical Society of Japan59, #2 (April 2007), pp. 335–356, Bibcode:2007PASJ...59..335T.
  9. 1 2 3 Fuhrmann, Klaus (2011). "Nearby stars of the Galactic disc and halo - V". Monthly Notices of the Royal Astronomical Society. 414 (4): 2893–2922. Bibcode:2011MNRAS.414.2893F. doi: 10.1111/j.1365-2966.2011.18476.x .
  10. 1 2 Maldonado, J.; et al. (October 2010), "A spectroscopy study of nearby late-type stars, possible members of stellar kinematic groups", Astronomy and Astrophysics, 521: A12, arXiv: 1007.1132 , Bibcode:2010A&A...521A..12M, doi:10.1051/0004-6361/201014948, S2CID   119209183.
  11. 1 2 Mamajek, Eric E.; Hillenbrand, Lynne A. (November 2008), "Improved Age Estimation for Solar-Type Dwarfs Using Activity-Rotation Diagnostics", The Astrophysical Journal, 687 (2): 1264–1293, arXiv: 0807.1686 , Bibcode:2008ApJ...687.1264M, doi:10.1086/591785, S2CID   27151456.
  12. ↑ Entry 01425+2016, The Washington Double Star Catalog Archived 2008-04-12 at the Wayback Machine , United States Naval Observatory. Accessed on line September 24, 2008.
  13. ↑ Halbwachs, J. -L; et al. (2018). "Multiplicity among solar-type stars. IV. The CORAVEL radial velocities and the spectroscopic orbits of nearby K dwarfs". Astronomy and Astrophysics. 619: A81. arXiv: 1808.04605 . Bibcode:2018A&A...619A..81H. doi:10.1051/0004-6361/201833377. S2CID   119437322.
  14. ↑ Wagman, M. (August 1987), "Flamsteed's Missing Stars", Journal for the History of Astronomy, 18 (3): 213, Bibcode:1987JHA....18..209W, doi:10.1177/002182868701800305, S2CID   118445625
  15. ↑ Bailer-Jones, C.A.L.; et al. (2018). "New stellar encounters discovered in the second Gaia data release". Astronomy & Astrophysics. 616: A37. arXiv: 1805.07581 . Bibcode:2018A&A...616A..37B. doi:10.1051/0004-6361/201833456. S2CID   56269929.
  16. ↑ HD 10476, database entry, The Geneva-Copenhagen Survey of Solar neighbourhood, J. Holmberg et al., 2007, CDS ID V/117A. Accessed on line November 19, 2008.
  17. ↑ Radick, Richard R.; et al. (March 2018). "Patterns of Variation for the Sun and Sun-like Stars". The Astrophysical Journal. 855 (2): 28. Bibcode:2018ApJ...855...75R. doi: 10.3847/1538-4357/aaaae3 . 75.
  18. ↑ Wright, J. T.; et al. (August 2008). "The Jupiter Twin HD 154345b". The Astrophysical Journal Letters. 683 (1): L63–L66. arXiv: 0802.1731 . Bibcode:2008ApJ...683L..63W. doi:10.1086/587461. S2CID   16808434.
  19. 1 2 Absil, O.; et al. (July 2013), "A near-infrared interferometric survey of debris-disc stars. III. First statistics based on 42 stars observed with CHARA/FLUOR", Astronomy and Astrophysics, 555: A104, arXiv: 1307.2488 , Bibcode:2013A&A...555A.104A, doi:10.1051/0004-6361/201321673, S2CID   16945896.
  20. ↑ Agati, J.-L.; et al. (February 2015), "Are the orbital poles of binary stars in the solar neighbourhood anisotropically distributed?", Astronomy and Astrophysics, 574: A6, arXiv: 1411.4919 , Bibcode:2015A&A...574A...6A, doi:10.1051/0004-6361/201323056, S2CID   55771565
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