A visual band light curve for CQ Tauri, plotted from INTEGRAL OMC data | |
Observation data Epoch J2000.0 Equinox J2000.0 | |
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Constellation | Taurus |
Right ascension | 05 35 58.467 |
Declination | 24° 44′ 54.09″ |
Apparent magnitude (V) | 10.48 (8.7 to 12.25) |
Characteristics | |
Evolutionary stage | Pre-main-sequence |
Spectral type | F5IVe |
B−V color index | 0.696±0.091 |
Variable type | Orion variable |
Astrometry | |
Radial velocity (Rv) | 22.60±2.7 km/s |
Proper motion (μ) | RA: 2.987 mas/yr Dec.: −26.364 mas/yr |
Parallax (π) | 6.6946 ± 0.0600 mas |
Distance | 487 ± 4 ly (149 ± 1 pc) |
Absolute magnitude (MV) | 5.92 |
Details | |
Mass | 1.67 M☉ |
Radius | 1.7 R☉ |
Luminosity | 10 L☉ |
Surface gravity (log g) | 4.0 cgs |
Temperature | 6,900 K |
Metallicity | +0.14 dex |
Rotational velocity (v sin i) | 105.0±5.0 km/s |
Age | 10 Myr |
Other designations | |
CQ Tau, BD+24°873, HD 36910, HIP 26295, SAO 77299, PPM 94541 | |
Database references | |
SIMBAD | data |
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.
This star was independently reported as a variable by Artjukinov (sp?) in 1948 and C. Hoffmeister in 1949. Hoffmeister classified it as a member of the RW Aurigae-like variables with a brightness that ranged from an apparent visual magnitude of 8.7 down to 10.5, making it one of the brightest members of that type. G. H. Herbig in 1960 found a spectral class of F2 for this star, and by 1973 it was classed as an Orion variable of the T Tauri type. In 1968, W. Götz and W. Wenzel discovered a faint emission of blue light coming from the system.
Spectral images of the system in 1973 showed double emission lines on an F-type star. It was found to be an infrared source by IRAS and associated with nebulosity, which allowed it to be cataloged as a Herbig Ae/Be star in 1994 by P. S. Thé and associates. The star undergoes irregular brightness decreases that are otherwise similar to an Algol-like variation. It is being orbited by an inhomogeneous accretion disk, which is the source for the emission lines.
CQ Tauri is a pre-main-sequence star with a stellar classification of F5IVe. It has 1.67 times the mass of the Sun and is radiating 10 times the Sun's luminosity with an effective temperature of 6,900 K. The star is about 10 million years old and is spinning with a projected rotational velocity of 105 km/s. Simulations intended to reproduce the distribution of the circumstellar disk suggest an embedded planet with a mass of 6–9 MJ is orbiting the star at a distance of ~20 AU. Near infrared observations in 2018 show a spiral structure in the disk that is consistent with the presence of an orbiting planet. However, no planet was detected.
Protoplanetary system
Observations with the Very Large Array during 2000 demonstrated the extent of the massive protoplanetary disk orbiting the star. The mass of dust in the disk was estimated at 1.5×10 M☉. Measurements suggest the dust grains in the disk around CQ Tauri have grown to a maximum of about a centimetre in size, with decreasing grain size beyond 40 AU from the host star. Data from the Atacama Large Millimeter Array show a cavity in the inner disk that is depleted of gas and dust. Isolated, thick clouds of dust are randomly obscuring the star.
In 2022, four spiral arms were detected in the protoplanetary disk. An as yet unseen planet on an eccentric and inclined orbit is suspected to be disturbing the shape of the disk.
References
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- Uyama, Taichi; et al. (March 2020), "Near-infrared Imaging of a Spiral in the CQ Tau Disk", The Astronomical Journal, 159 (3): 9, arXiv:1910.07605, Bibcode:2020AJ....159..118U, doi:10.3847/1538-3881/ab7006, S2CID 204743781, 118.
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- Hammond, Iain; Christiaens, Valentin; Price, Daniel J.; Ubeira-Gabellini, Maria Giulia; Baird, Jennifer; Calcino, Josh; Benisty, Myriam; Lodato, Giuseppe; Testi, Leonardo; Pinte, Christophe; Toci, Claudia; Fedele, Davide (2022), "External or internal companion exciting the spiral arms in CQ Tau?", Monthly Notices of the Royal Astronomical Society, 515 (4): 6109–6121, arXiv:2207.08587, doi:10.1093/mnras/stac2119
Further reading
- Safonov, Boris S.; et al. (January 2022), "Apparent Motion of the Circumstellar Envelope of CQ Tau in Scattered Light", The Astronomical Journal, 163 (1): 31, arXiv:2111.02726, Bibcode:2022AJ....163...31S, doi:10.3847/1538-3881/ac36cb, S2CID 242757117, 31.
- Wölfer, L.; et al. (April 2021), "A highly non-Keplerian protoplanetary disc. Spiral structure in the gas disc of CQ Tau", Astronomy & Astrophysics, 648, arXiv:2012.04680, Bibcode:2021A&A...648A..19W, doi:10.1051/0004-6361/202039469, S2CID 228064514, A19.
- Assani, K. (January 2020), "Variability in the Gas and Dust Emission of the UX Orioni Star CQ Tau", Bulletin of the American Astronomical Society, 52 (1), Bibcode:2020AAS...23545101A.
- Ubeira Gabellini, Maria Giulia (December 2018), "The gas and dust disk around the CQ Tau pre-main sequence star", Protoplanetary disks seen through the eyes of new-generation high-resolution instruments. Proceedings of the conference held 25–28 June 2018 in Rome, Italy, p. 30, Bibcode:2018ppd..confE..30U, doi:10.5281/zenodo.1893261.
- Tax, Tomáš (November 2018), "Asymmetric CQ-Tau Transition Disk at High Angular Resolution", Take a Closer Look, 15–19 October 2018 in ESO-HQ, Garching b. München, Germany, p. 112, Bibcode:2018tcl..confE.112T, doi:10.5281/zenodo.1488994.
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- Chapillon, E.; et al. (September 2010), "C I observations in the CQ Tauri proto-planetary disk: evidence of a very low gas-to-dust ratio?", Astronomy and Astrophysics, 520: A61, arXiv:1006.5244, Bibcode:2010A&A...520A..61C, doi:10.1051/0004-6361/201014841, S2CID 119177523, A61.
- Chapillon, E.; et al. (November 2008), Charbonnel, C.; et al. (eds.), "Disks around CQ Tau and MWC 758: Dense PDRs or gas dispersal?", SF2A-2008: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics, p. 303, Bibcode:2008sf2a.conf..303C.
- Kozlova, O. V.; et al. (January 2007), "Structure of the inner region of the accretion disk of the Herbig Ae star CQ Tau based on long-term monitoring data", Astrophysics, 50 (1): 26–39, Bibcode:2007Ap.....50...26K, doi:10.1007/s10511-007-0004-z, S2CID 120401305.
- Doucet, C.; et al. (December 2006), "Mid-infrared imaging of the circumstellar dust around three Herbig Ae stars: HD 135344, CQ Tau, and HD 163296", Astronomy and Astrophysics, 460 (1): 117–124, arXiv:astro-ph/0608615, Bibcode:2006A&A...460..117D, doi:10.1051/0004-6361:20054371, S2CID 1722324.
- Shakhovskoj, D. N.; et al. (April 2005), "Analysis of the Historical Light Curve of the UX Ori Star CQ Tau", Astrophysics, 48 (2): 135–142, Bibcode:2005Ap.....48..135S, doi:10.1007/s10511-005-0014-7, S2CID 121443460.
- Shakhovskoy, D. N.; et al. (2005), "Variations of Effective Size of Dust Grains in CQ Tau", Protostars and Planets V, Proceedings of the Conference held October 24–28, 2005, in Hilton Waikoloa Village, Hawai'i. LPI Contribution No. 1286, no. 1286, p. 8119, Bibcode:2005prpl.conf.8119S.
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