Contents

TZ Arietis

Nearby red dwarf star in the constellation Aries

TZ Arietis

TZ Arietis Location of TZ Arietis in the constellation Aries
Observation data Epoch J2000      Equinox J2000
Constellation	Aries
Right ascension	02h00m 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 constellationofAries. 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.

Variability[edit]

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[edit]

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]

See also[edit]

• List of nearest stars and brown dwarfs

References[edit]

Notes[edit]

Further reading[edit]

• Harrington, R. S.; Dahn, C. C. (April 1980), "Summary of U.S. Naval Observatory parallaxes", Astronomical Journal, 85: 454–465, Bibcode:1980AJ.....85..454H, doi:10.1086/112696.
• Riaz, Basmah; Gizis, John E.; Harvin, James (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 Table 1.
• Dittmann, Jason A.; Irwin, Jonathan M.; Charbonneau, David; Berta-Thompson, Zachory K. (2014), "Trigonometric Parallaxes for 1507 Nearby Mid-to-late M Dwarfs", The Astrophysical Journal, 784 (2): 156, arXiv:1312.3241, Bibcode:2014ApJ...784..156D, doi:10.1088/0004-637X/784/2/156, S2CID 18789867 Table with parallaxes.

External links[edit]

• ARICNS entry Archived 2007-06-10 at the Wayback Machine
• luyten-1159-16
• Image luyten-1159-16
• GJ 83.1
• Image TZ Arietis