CVSO 30

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CVSO 30
VLT Snaps An Exotic Exoplanet "First".tif
VLT image of CVSO 30 and its planet, CVSO 30 c
Observation data
Epoch J2000.0        Equinox J2000.0
Constellation Orion [1]
Right ascension 05h 25m 07.557s [2]
Declination +01° 34′ 24.36″ [2]
Apparent magnitude  (V)+16.26 [3]
Characteristics
Evolutionary stage pre-main sequence [3]
Spectral type M3 [3]
Variable type T Tau [3]
Astrometry
Proper motion (μ)RA: +1.274 [2] mas/yr
Dec.: −0.364 [2] mas/yr
Parallax (π)2.9403±0.0372  mas [2]
Distance 1,110 ± 10  ly
(340 ± 4  pc)
Details
Mass 0.39 ± 0.05 [3]   M☉
Radius 1.39 [3]   R☉
Temperature 3470 [3]   K
Age 2.65 [4]   Myr
Other designations
2MASS J05250755+0134243, PTFO 8-8695 [5]
Database references
SIMBAD data

CVSO 30 (PTFO 8-8695) is a suspected binary T Tauri star, located in constellation Orion at 1200 light years from Earth with one candidate planet called CVSO 30 c. The candidate planet is a gas giant. The star is named after the CIDA Variability Survey of Orion (CVSO) [6] and the Palomar Transient Factory (PTF) and is within the 25 Ori group. [7]

Contents

Planetary system

The CVSO 30 planetary system [8]
Companion
(in order from star)		 Mass Semimajor axis
(AU)		 Orbital period
(years)		 Eccentricity Inclination Radius
c (unconfirmed)4.7 +5.5
−2.0 MJ 		66027000——1.63 +0.87
−0.34  RJ

CVSO 30 may have one planet called CVSO 30 c. CVSO 30 c is calculated to have a period of 27,000 years and a semimajor axis of 660 AU.

Direct imaging of the suspected CVSO 30 c, with a calculated mass equal to 4.7 Jupiter's, has been achieved through photometric and spectroscopic high contrast observations carried out with the Very Large Telescope located in Chile, the Keck Observatory in Hawaii and the Calar Alto Observatory in Spain. [9] However, the colors of the object suggest that it may actually be a background star, such as a K-type giant or a M-type subdwarf. [10]

Light curves for CVSO 30, adapted from Koen (2021) CVSO30LightCurve.png
Light curves for CVSO 30, adapted from Koen (2021)

By 2020, the phase of "dips" caused by suspected planet CVSO 30 b had drifted nearly 180 degrees from the expected value, thus ruling out the existence of the planet. Instead, a rare type of stellar starspot activity with very large starspots is now suspected. Also, CVSO 30 is suspected to be a stellar binary, with the previously reported planetary orbital period equal to the rotation period of the companion star. [12] Further investigation of "dips" by 2022 led to hypothesis of a large gas cloud close to synchronous orbit, dust would likely sublimate. [13]

References

  1. ↑ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific . 99 (617): 695. Bibcode:1987PASP...99..695R. doi: 10.1086/132034 . Constellation record for this object at VizieR.
  2. 1 2 3 4 5 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.
  3. 1 2 3 4 5 6 7 Van Eyken, Julian C.; et al. (2012). "The Ptf Orion Project: A Possible Planet Transiting a T-Tauri Star". The Astrophysical Journal. 755 (1): 42. arXiv: 1206.1510 . Bibcode:2012ApJ...755...42V. doi:10.1088/0004-637X/755/1/42. S2CID   2753064.
  4. ↑ "Extrasolar Planets Encyclopaedia". Archived from the original on 19 February 2019. Retrieved 15 November 2016.
  5. ↑ "CVSO 30". SIMBAD . Centre de données astronomiques de Strasbourg . Retrieved 5 October 2018.
  6. ↑ Briceño, Cesar; Calvet, Nuria; Hernández, J.; Vivas, A. K.; Hartmann, Lee; Downes, J. J.; Berlind, Perry (February 2005). "The CIDA Variability Survey of Orion OB1. I. The Low-Mass Population of Ori OB1a and 1b". The Astronomical Journal. 129 (2): 907–926. arXiv: astro-ph/0410521 . Bibcode:2005AJ....129..907B. doi:10.1086/426911. ISSN   0004-6256.
  7. ↑ Briceno, Cesar; Hartmann, Lee; Hernandez, Jesus; Calvet, Nuria; Vivas, A. Katherina; Furesz, Gabor; Szentgyorgyi, Andrew (June 2007). "25 Orionis: A Kinematically Distinct 10 Myr Old Group in Orion OB1a". The Astrophysical Journal. 661 (2): 1119–1128. arXiv: astro-ph/0701710 . Bibcode:2007ApJ...661.1119B. doi:10.1086/513087. ISSN   0004-637X.
  8. ↑ Schmidt, T. O. B.; Neuhäuser, R.; Briceño, C.; Vogt, N.; Raetz, St.; Seifahrt, A.; Ginski, C.; Mugrauer, M.; Buder, S.; Adam, C.; Hauschildt, P.; Witte, S.; Helling, Ch.; Schmitt, J. H. M. M. (September 2016). "Direct Imaging discovery of a second planet candidate around the possibly transiting planet host CVSO 30". Astronomy & Astrophysics. 593: A75. arXiv: 1605.05315 . Bibcode:2016A&A...593A..75S. doi:10.1051/0004-6361/201526326. ISSN   0004-6361.
  9. ↑ "Amazing Photo Shows Likely Alien Planet 1,200 Light-Years Away". MSN. 21 June 2016. Archived from the original on 11 August 2016. Retrieved 22 June 2016.
  10. ↑ Lee, Chien-Hsiu; Chiang, Po-Shih (2018). "Evidence that the Planetary Candidate CVSO30c is a Background Star from Optical, Seeing-limited Data". The Astrophysical Journal. 852 (2): L24. arXiv: 1712.08727 . Bibcode:2018ApJ...852L..24L. doi: 10.3847/2041-8213/aaa40b . S2CID   119270170.
  11. ↑ Koen, C. (March 2021). "Starspot modelling of the TESS light curve of CVSO 30". Astronomy and Astrophysics. 647: L1. Bibcode:2021A&A...647L...1K. doi: 10.1051/0004-6361/202140400 . hdl: 10566/6123 .
  12. ↑ Koen, C.; et al. (2020). "Properties of CVSO 30 from TESS measurements: Probably a binary T Tauri star with complex light curves and no obvious planets". Monthly Notices of the Royal Astronomical Society. 494 (3): 4349–4356. arXiv: 2005.10253 . doi: 10.1093/mnras/staa1038 .
  13. ↑ Bischoff, R.; et al. (2022). "YETI follow-up observations of the T Tauri star CVSO 30 with transit-like dips". Monthly Notices of the Royal Astronomical Society. arXiv: 2201.12405 . doi: 10.1093/mnras/stac293 .

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