TZ Arietis

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TZ Arietis
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TZ Arietis
Location of TZ Arietis in the constellation Aries

Observation data
Epoch J2000       Equinox J2000
Constellation Aries
Right ascension 02h 00m 12.95632s [1]
Declination +13° 03′ 07.0006″ [1]
Apparent magnitude  (V)12.298 [2]
Characteristics
Spectral type M4.5 V [3]
U−B color index +1.37 [4]
B−V color index +1.80 [4]
R−I color index 1.39 [3]
Variable type Flare star
Astrometry
Radial velocity (Rv)−28.29±0.25 [1]  km/s
Proper motion (μ)RA: 1096.458  mas/yr [1]
Dec.: -1771.526  mas/yr [1]
Parallax (π)223.7321 ± 0.0699  mas [1]
Distance 14.578 ± 0.005  ly
(4.470 ± 0.001  pc)
Absolute magnitude  (MV)14.03 [5]
Details
Mass 0.14 [6]   M☉
Radius 0.161 [7]   R☉
Luminosity 0.00135 [8]   L☉
Surface gravity (log g)5.05 [6]   cgs
Temperature 3,158 [7]   K
Metallicity [Fe/H]−0.14 [7]   dex
Rotational velocity (v sin i)3.8 [8]  km/s
Age 4.8 [6]   Gyr
Other designations
TZ Ari, GJ  83.1, GJ 9066, G 003-033, L  1159-16, LFT  171, LHS  11, PLX  412.02, 2MASS J02001278+1303112 [9]
Database references
SIMBAD data

TZ Arietis (also known as Gliese 83.1, GJ 9066, or L 1159-16) is a red dwarf in the northern constellation of Aries. With a normal apparent visual magnitude of 12.3, it is too faint to be seen by the naked eye, although it lies relatively close to the Sun at a distance of 14.6 light-years (4.47 parsecs ). It is a flare star, which means it can suddenly increase in brightness for short periods of time.

Contents

Variability

TZ Arietis is a variable star. It is a flare star, showing brief increases in brightness due to eruptions from its surface. In the ultraviolet, flares of over a magnitude have been observed. In addition it shows longterm variations in brightness which may be due to starspots and rotation, possibly classifying it as a BY Draconis variable. [10] It was given the variable star designation TZ Arietis in 1970. [11]

Planetary system

In a preprint submitted to arXiv in June 2019, three candidate planets were reported in orbit around this star (GJ 83.1) with orbital periods of 2, 240, and 770 days. [12] A paper published in August 2020 reported a confirmation of the 240-day and 770-day planets, designating them "b" and "c", respectively. [13]

In March 2022, astronomers using the Calar Alto Observatory in Spain, as part of the CARMENES survey project, reported an independent confirmation of the 770-day planet, which they designated "b". However, they found no evidence for the 240-day planet, and confidently defined the 2-day candidate as nothing more than a spurious chromatic effect of the star, linked to its rotation. [14] The NASA Exoplanet Archive still refers to the confirmed, 770-day planet as "c". [15]

The TZ Arietis planetary system [14]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(days)		 Eccentricity Inclination Radius
b [note 1] ≥0.21±0.02  MJ 0.88±0.02771.36+1.34
−1.23		0.46±0.04——

See also

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References

  1. 1 2 3 4 5 6 Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv: 2208.00211 . Bibcode:2023A&A...674A...1G. doi: 10.1051/0004-6361/202243940 . S2CID   244398875. Gaia DR3 record for this source at VizieR.
  2. ↑ Landolt, Arlo U. (July 1992), "UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator", Astronomical Journal, 104 (1): 340–371, 436–491, Bibcode:1992AJ....104..340L, doi: 10.1086/116242 .
  3. 1 2 Riaz, Basmah; Gizis, John E.; Harvin, James (August 2006), "Identification of New M Dwarfs in the Solar Neighborhood", The Astronomical Journal, 132 (2): 866–872, arXiv: astro-ph/0606617 , Bibcode:2006AJ....132..866R, doi:10.1086/505632, S2CID   6282011.
  4. 1 2 Nicolet, B. (1978), "Photoelectric photometric Catalogue of homogeneous measurements in the UBV System", Astronomy and Astrophysics Supplement Series, 34: 1–49, Bibcode:1978A&AS...34....1N.
  5. ↑ Boro Saikia, S.; et al. (2018), "Chromospheric activity catalogue of 4454 cool stars. Questioning the active branch of stellar activity cycles", Astronomy and Astrophysics, 616: A108, arXiv: 1803.11123 , Bibcode:2018A&A...616A.108B, doi:10.1051/0004-6361/201629518, S2CID   118915212.
  6. 1 2 3 Yee, Samuel W.; Petigura, Erik A.; von Braun, Kaspar (2017), "Precision Stellar Characterization of FGKM Stars using an Empirical Spectral Library", The Astrophysical Journal, 836 (1): 77, arXiv: 1701.00922 , Bibcode:2017ApJ...836...77Y, doi: 10.3847/1538-4357/836/1/77 , S2CID   6302522.
  7. 1 2 3 Houdebine, Éric R.; Mullan, D. J.; Doyle, J. G.; de la Vieuville, Geoffroy; Butler, C. J.; Paletou, F. (2019), "The Mass–Activity Relationships in M and K Dwarfs. I. Stellar Parameters of Our Sample of M and K Dwarfs", The Astronomical Journal, 158 (2): 56, arXiv: 1905.07921 , Bibcode:2019AJ....158...56H, doi: 10.3847/1538-3881/ab23fe , S2CID   159041104.
  8. 1 2 McLean, M.; Berger, E.; Reiners, Ansgar (February 2012), "The Radio Activity-Rotation Relation of Ultracool Dwarfs", The Astrophysical Journal, 746 (1): 23, arXiv: 1108.0415 , Bibcode:2012ApJ...746...23M, doi:10.1088/0004-637X/746/1/23, S2CID   119159519.
  9. ↑ "TZ Ari -- Flare Star", SIMBAD Astronomical Database, Centre de Données astronomiques de Strasbourg , retrieved 2012-08-18.
  10. ↑ Gershberg, R. E.; Katsova, M. M.; Lovkaya, M. N.; Terebizh, A. V.; Shakhovskaya, N. I. (1999), "Catalogue and bibliography of the UV Cet-type flare stars and related objects in the solar vicinity", Astronomy and Astrophysics Supplement Series, 139 (3): 555–558, Bibcode:1999A&AS..139..555G, doi: 10.1051/aas:1999407 .
  11. ↑ Kukarkin, B. V.; Kholopov, P. N.; Perova, N. B. (October 1970), "57th Name-List of Variable Stars", Information Bulletin on Variable Stars, 480 (1): 1, Bibcode:1970IBVS..480....1K.
  12. ↑ Barnes, J. R.; et al. (2019-06-11), Frequency of planets orbiting M dwarfs in the Solar neighbourhood, arXiv: 1906.04644 .
  13. ↑ Feng, Fabo; Shectman, Stephen A.; Clement, Matthew S.; Vogt, Steven S.; Tuomi, Mikko; Teske, Johanna K.; Burt, Jennifer; Crane, Jeffrey D.; Holden, Bradford; Wang, Sharon Xuesong; Thompson, Ian B.; Díaz, Matías R.; Butler, R. Paul (2020), "Search for Nearby Earth Analogs .III. Detection of 10 New Planets, 3 Planet Candidates, and Confirmation of 3 Planets around 11 Nearby M Dwarfs", The Astrophysical Journal Supplement Series, 250 (2): 29, arXiv: 2008.07998 , Bibcode:2020ApJS..250...29F, doi: 10.3847/1538-4365/abb139 , S2CID   221150644.
  14. 1 2 Quirrenbach, A.; et al. (2022), "The CARMENES search for exoplanets around M dwarfs", Astronomy & Astrophysics, 663: A48, arXiv: 2203.16504 , Bibcode:2022A&A...663A..48Q, doi:10.1051/0004-6361/202142915, S2CID   247835988.
  15. ↑ "GJ 9066". NASA Exoplanet Archive . Retrieved 27 September 2022.

Notes

  1. ↑ Referred to as c by some sources.

Further reading

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