XZ Tauri

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XZ Tauri
XZTauLightCurve.png
A visual band light curve for XZ Tauri. The main plot shows the long-term variability, and the inset shows the year 2000 superflare on the north star. Adapted from Dodin et al. (2016) [1] and Coffey et al. (2004). [2]
Observation data
Epoch J2000.0       Equinox J2000.0
Constellation Taurus
Right ascension 04h 31m 40.08690s [3]
Declination +18° 13′ 56.6424″ [3]
Apparent magnitude  (V)10.40 [4]
Characteristics
Spectral type M2.0 + M3.5 [5]
Astrometry
Proper motion (μ)RA: 9.1 [6]   mas/yr
Dec.: −17.8 [6]   mas/yr
Distance 460  ly
(140 [7]   pc)
Orbit [8]
PrimaryA [lower-alpha 1]
CompanionB
Period (P)155 yr
Semi-major axis (a)0.172+0.002
−0.003″
Eccentricity (e)0.742+0.025
−0.034
Inclination (i)0.0°
Argument of periastron (ω)
(secondary)		−42.2+2.0
−4.7°
Details [5]
A [lower-alpha 1]
Mass 0.37  M☉
Radius 1.1  R☉
Luminosity 0.17  L☉
B
Mass 0.29  M☉
Radius 1.7  R☉
Luminosity0.31  L☉
Temperature 3,550 [7]   K
Age 4.6 [7]   Myr
Other designations
XZ Tau, GSC  01269-00171 [9]
Database references
SIMBAD data

XZ Tauri is a binary system approximately 460 light-years away in the constellation Taurus. The system consists of two T Tauri stars orbiting each other about 6 billion kilometers apart (roughly the same distance as Pluto is from the Sun). The system made news in 2000 when a superflare was observed in the system.

Contents

A third star, component C, has been observed at a separation of 0.09″ , but subsequent observations failed to find it. [10] [8] The T Tauri star HL Tauri, 23″ away, is also sometimes listed as a companion. [9]

Notes

  1. 1 2 Sources vary on their definitions of the primary and secondary components. A is defined here as the more massive component, with a lower temperature but higher luminosity. Other sources refer to the components as north and south, [lower-alpha 2] or Aa and Ab. [lower-alpha 3] The southerly star Ab is generally brighter at optical wavelengths and more massive, but is less luminous.

Related Research Articles

<span class="mw-page-title-main">Protoplanetary disk</span> Gas and dust surrounding a newly formed star

A protoplanetary disk is a rotating circumstellar disc of dense gas and dust surrounding a young newly formed star, a T Tauri star, or Herbig Ae/Be star. The protoplanetary disk may also be considered an accretion disk for the star itself, because gases or other material may be falling from the inner edge of the disk onto the surface of the star. This process should not be confused with the accretion process thought to build up the planets themselves. Externally illuminated photo-evaporating protoplanetary disks are called proplyds.

<span class="mw-page-title-main">V1057 Cygni</span> Star in the constellation Cygnus

V1057 Cygni is a suspected binary star system in the northern constellation of Cygnus. It is a variable star of the FU Orionis-type, and was the second FU Orionis-type variable to be discovered. The system is located at a distance of approximately 3,000 light years from the Sun, in the North America Nebula. It has an apparent visual magnitude of around 12.4.

<span class="mw-page-title-main">AA Tauri</span> Star in the constellation Taurus

AA Tauri is a young variable star in the equatorial constellation of Taurus, located in the Taurus-Auriga star-forming region. It is too faint to view with the naked eye, having an apparent visual magnitude that varies from 12.2 down to 16.1. The star is located approximately 439 light-years away from the Sun based on parallax, and is drifting further away with a radial velocity of +17 km/s.

<span class="mw-page-title-main">Taurus molecular cloud</span> Interstellar molecular cloud in the constellations Taurus and Auriga

The Taurus molecular cloud (TMC-1) is an interstellar molecular cloud in the constellations Taurus and Auriga. This cloud hosts a stellar nursery containing hundreds of newly formed stars. The Taurus molecular cloud is only 140 pc away from Earth, making it possibly the nearest large star formation region. It has been important in star formation studies at all wavelengths.

<span class="mw-page-title-main">LkCa 15</span> Star system in the constellation Taurus

LkCa 15 is a T Tauri star in the Taurus Molecular Cloud. These types of stars are relatively young pre-main-sequence stars that show irregular variations in brightness. It has a mass that is about 97% of the Sun, an effective temperature of 4370 K, and is slightly cooler than the Sun. Its apparent magnitude is 11.91, meaning it is not visible to the naked eye.

<span class="mw-page-title-main">GG Tauri</span> Star in the constellation Taurus

GG Tauri, often abbreviated as GG Tau, is a quintuple star system in the constellation Taurus. At a distance of about 450 light years away, it is located within the Taurus-Auriga Star Forming Region. The system comprises three stars orbiting each other in a hierarchical triple system, known as GG Tauri A, and another binary star system more distant from the central system, known as GG Tauri B.

<span class="mw-page-title-main">GW Orionis</span> Star in the constellation Orion

GW Orionis is a T Tauri type pre-main sequence hierarchical triple star system. It is associated with the Lambda Orionis star-forming region and has an extended circumtrinary protoplanetary disk.

<span class="mw-page-title-main">CI Tauri</span> Star in the constellation Taurus

CI Tauri is a young star, about 2 million years old, located approximately 500 light years away in the constellation Taurus. It is still accreting material from a debris disk at an unsteady pace, possibly modulated by the eccentric orbital motion of the inner planet. The spectral signatures of compounds of sulfur were detected from the disk.

<span class="mw-page-title-main">DH Tauri</span> Star in the constellation Taurus

DH Tauri, also known as DH Tau, is a type M star, located 140 parsecs away. It forms a binary system with DI Tauri 15″ away, and has a substellar companion, either a brown dwarf or massive exoplanet.

<span class="mw-page-title-main">AK Scorpii</span> Binary star in the constellation Scorpius

AK Scorpii is a Herbig Ae/Be star and spectroscopic binary star about 459 light-years distant in the constellation Scorpius. The star belongs to the nearby Upper Centaurus–Lupus star-forming region and the star is actively accreting material. The binary is surrounded by a circumbinary disk that was imaged with VLT/SPHERE in scattered light and with ALMA.

<span class="mw-page-title-main">RW Aurigae</span> Young binary star system in the constellation Auriga

RW Aurigae is a young binary system in the constellation of Auriga about 530 light years away, belonging to the Taurus-Auriga association of the Taurus Molecular Cloud. RW Aurigae B was discovered in 1944.

<span class="mw-page-title-main">RY Tauri</span> Star in the constellation Taurus

RY Tauri is a young T Tauri star in the constellation of Taurus about 450 light years away, belonging to the Taurus Molecular Cloud. It is more massive than typical T Tauri stars, and may be an intermediate between this class and the Herbig Ae/Be star type.

<span class="mw-page-title-main">BP Tauri</span> Star in the constellation Taurus

BP Tauri is a young T Tauri star in the constellation of Taurus about 416 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">HK Tauri</span> Young binary star system in the constellation of Taurus

HK Tauri is a young binary star system in the constellation of Taurus about 434 light-years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">GI Tauri and GK Tauri</span> Binary star system in the constellation of Taurus

GK Tauri is a young T Tauri-type pre-main sequence star in the constellation of Taurus about 421 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">GV Tauri</span> Young binary star system in the constellation of Taurus

GK Tauri is a young binary system composed of T Tauri-type pre-main sequence stars in the constellation of Taurus about 466 light years away, belonging to the Taurus Molecular Cloud.

<span class="mw-page-title-main">DL Tauri</span> Protostar system with planetary system in the constellation of Taurus

DL Tauri is a young T Tauri-type pre-main sequence stars in the constellation of Taurus about 522 light years away, belonging to the Taurus Molecular Cloud. It is partially obscured by the foreground gas cloud rich in carbon monoxide, and is still accreting mass, producing 0.14 L☉ due to release of accretion energy. The stellar spectrum shows the lines of ionized oxygen, nitrogen, sulfur and iron.

<span class="mw-page-title-main">HD 283572</span> Young star in constellation Taurus

HD 283572 is a young T Tauri-type pre-main sequence star in the constellation of Taurus about 414 light years away, belonging to the Taurus Molecular Cloud. It is a rather evolved protostar which already dispersed its birth shroud. The star emits a very high X-ray flux of 1031 ergs/s. That radiation flux associated with the magnetic activity induced a high coronal temperature of 3 kEv and regular flares. HD 283572 will eventually evolve to an A-type main-sequence star when on the main sequence. It is no longer accreting mass, and is magnetically decoupled from the remnants of the protoplanetary disk, belonging to the terminal, 3rd phase of the disk evolution.

<span class="mw-page-title-main">CQ Tauri</span> Star in the constellation Taurus

CQ Tauri is a young variable star in the equatorial constellation of Taurus. It is too faint to be visible to the naked eye with an apparent visual magnitude that ranges from 8.7 to 12.25. The distance to this star is approximately 487 light years based on parallax measurements, and it is drifting further away with a radial velocity of ~23 km/s. It appears to be part of the T-association Tau 4. CQ Tauri lies close enough to the ecliptic to undergo lunar occultations.

<span class="mw-page-title-main">IM Lupi</span> Pre-main-sequence star in the constellation Lupus

IM Lupi is a young stellar object with a surrounding protoplanetary disk. The young star is suspected to host a still forming protoplanet at a distance of 110 astronomical units (AU) and a mass of 2-3 MJ. IM Lupi is 508 light-years distant.

References

  1. ↑ Dodin, A. V.; Emelyanov, N. V.; Zharova, A. V.; Lamzin, S. A.; Malogolovets, E. V.; Roe, J. M. (January 2016). "Orbital motions and light curves of young binaries XZ Tau and VY Tau". Astronomy Letters. 42 (1): 29–40. arXiv: 1509.04966 . Bibcode:2016AstL...42...29D. doi:10.1134/S1063773716010035. S2CID   118495210.
  2. ↑ Coffey, D.; Downes, T. P.; Ray, T. P. (May 2004). "The evolution and simulation of the outburst from XZ Tauri – A possible EXor?". Astronomy and Astrophysics. 419 (2): 593–598. arXiv: astro-ph/0402635 . Bibcode:2004A&A...419..593C. doi: 10.1051/0004-6361:20034316 . S2CID   17421498.
  3. 1 2 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.
  4. ↑ Ducati, J. R. (2002). "VizieR Online Data Catalog: Catalogue of Stellar Photometry in Johnson's 11-color system". CDS/ADC Collection of Electronic Catalogues. 2237. Bibcode:2002yCat.2237....0D.
  5. 1 2 Hartigan, Patrick; Kenyon, Scott J. (January 2003). "A Spectroscopic Survey of Subarcsecond Binaries in the Taurus-Auriga Dark Cloud with the Hubble Space Telescope". The Astrophysical Journal. 583 (1): 334–357. arXiv: astro-ph/0209608 . Bibcode:2003ApJ...583..334H. doi:10.1086/345293. S2CID   10433035.
  6. 1 2 Zacharias, N.; Urban, S. E.; Zacharias, M. I.; Wycoff, G. L.; Hall, D. M.; Germain, M. E.; Holdenried, E. R.; Winter, L. (2003). "UCAC2 Catalogue (Zacharias+ 2004)". Vizier Online Data Catalog. Bibcode:2003yCat.1289....0Z.
  7. 1 2 3 Osorio, Mayra; et al. (July 2016). "A Dwarf Transitional Protoplanetary Disk around XZ Tau B". The Astrophysical Journal Letters. 825 (1): 6. arXiv: 1606.03118 . Bibcode:2016ApJ...825L..10O. doi: 10.3847/2041-8205/825/1/L10 . S2CID   59585588. L10.
  8. 1 2 Ichikawa, Takanori; Kido, Miyu; Takaishi, Daisuke; Shimajiri, Yoshito; Tsukamoto, Yusuke; Takakuwa, Shigehisa (2021). "Misaligned Circumstellar Disks and Orbital Motion of the Young Binary XZ Tau". The Astrophysical Journal. 919 (1): 55. arXiv: 2106.11924 . Bibcode:2021ApJ...919...55I. doi: 10.3847/1538-4357/ac0dc3 . S2CID   235593373.
  9. 1 2 "XZ Tau". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 2020-12-09.
  10. ↑ Osorio, Mayra; MacÍas, Enrique; Anglada, Guillem; Carrasco-González, Carlos; Galván-Madrid, Roberto; Zapata, Luis; Calvet, Nuria; Gómez, José F.; Nagel, Erick; Rodríguez, Luis F.; Torrelles, José M.; Zhu, Zhaohuan (2016). "A Dwarf Transitional Protoplanetary Disk Around Xz Tau B". The Astrophysical Journal. 825 (1): L10. arXiv: 1606.03118 . Bibcode:2016ApJ...825L..10O. doi: 10.3847/2041-8205/825/1/L10 . S2CID   59585588.
  11. ↑ "Jets, bubbles, and bursts of light in Taurus". www.spacetelescope.org. ESA/Hubble. Retrieved 6 November 2014.
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