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SR 12 (star)

SR 12

SR 12 and SR 12c (lower left) with JWST MIRI
Observation data
Epoch J2000      Equinox J2000
Constellation Ophiuchus
Right ascension 16h 27m 19.51s
Declination −24° 41′ 40.41″
Apparent magnitude (V) 13.09 to 13.53[1]
Characteristics
Evolutionary stage T-Tauri binary
Spectral type M3+M8[2]
Variable type rotational variable[3]
Astrometry
Radial velocity (Rv)-5.648320 ±0.01018[4] km/s
Proper motion (μ) RA: -7.703 ±1.088 mas/yr[5]
Dec.: -25.327 ±0.829 mas/yr[5]
Parallax (π)8.9034 ± 0.4288 mas[5]
Distance370 ± 20 ly
(112 ± 5 pc)
Details
SR 12A
Mass0.36+0.16
−0.07[3] M☉
Radius2.0 ±0.3[3] R☉
Temperature3428[6] K
Rotation3.4 to 3.6 days[1]
Age2[2] Myr
SR 12B
Temperature2500[6] K
Position (relative to SR 12A)[7]
ComponentSR 12B
Epoch of observation2022.2827
Angular distance0.1118 ±1.1″
Position angle76.2 ±1.1°
Other designations
EM* SR 12, 2MASS J16271951-2441403, ISO-Oph 130, ROX 21, TIC 175629526, V* V2247 Oph, WDS J16273-2442AB
Database references
SIMBADdata
Exoplanet Archivedata

SR 12 (also known as V2247 Oph) is a weak-line T-Tauri binary that has a planetary-mass companion with a detected accretion disk.[2]

The binary

SR 12 was discovered by Otto Struve and Mogens Rudkjøbing in 1949 as an emission-line star with a spectral type of M. The first letters of their names were used to name the star, together with the star number in their catalog.[8] It was also observed as an x-ray source with the Einstein Observatory, having the designation ROX 21.[9] The binary was discovered with the help of lunar occultations and speckle interferometry in 1987.[10]

The binary is located in the ρ Ophiuchi star-forming region and is a weak-line T-Tauri binary, meaning it still accretes gaseous material from a circumstellar disk.[6] There are differences in spectral type classifications of the individual stars.[2] A K4/M2.5 binary was suggested,[11] as well as a M3+M8 binary.[6][2] The binary is separated by about 0.21 arcseconds,[12] which corresponds to a separation of 24 AU.[2] Speckle interferometry from SOAR does however find a lower separation of 0.1118 ±1.1 arcseconds.[7]

The star is a variable with a rotation period that changes between 3.4 and 3.6 days. This is due to stellar spots at different latitudes corresponding to different rotation periods, which indicates photospheric shearing.[1][3] The magnetic surface of the primary was mapped in 2010. The magnetic field showed changes within 1 week. Excess emissions concentrated at mid-latitude are seen as a footprint of an accretion funnel.[3] The binary does not have any detection of circumbinary dust from Spitzer and ALMA observations.[2]

Planetary system

SR 12c was first detected in 2002 using the Infrared Survey Facility (IRSF), which was constructed and operated by Nagoya University and NAOJ and is located at the South African Astronomical Observatory. Follow-up observations were carried out with the Subaru Telescope in 2005 and 2008. Archival Hubble Space Telescope and Very Large Telescope (VLT) data were used to confirm the astrometry.[12] The companion is also mentioned in a paper from 2002 that detects it in Hubble/NICMOS.[13]

SR 12c has a separation of about 980 AU from the binary.[2] The near-infrared spectrum suggested a spectral type of M9.0 ± 0.5 of the planetary-mass companion (PMC) and a mass of 14+7
−8 MJ.[12] An additional higher-resolution near-infrared spectrum was taken in 2014, which showed signs of very low surface gravity, which is an indicator of youth.[14] VLT spectroscopy resulted in a spectral type of L0 ± 1.[15] A later work found that SR 12c is less massive with 11 ±3 MJ and SED-fitting yielded a spectral type of L0 ±1.[2] Several observations indicated that SR 12c is surrounded by a disk.

Observations with the VLT X-SHOOTER showed hydrogen emission lines, especially Hydrogen-alpha. This indicated that SR 12c accretes material at a rate of 10−11.08±0.40 M☉/year.[15][16] The object also showed infrared excess from Spitzer IRAC photometry.[17] Observations with ALMA did detect the disk, but was not able to resolve the disk, indicating a dust disk radius less than 5 AU and the radius might be about 0.3 AU if the continuum is optically thick. The disk has a dust mass twice as high as the disk around PDS 70c, but is less massive than OTS 44. Assuming the disk has only 1 mm grains, the dust mass of the disk is 0.012 ME (0.95 ML). For a disk only made of 1 μm grains, it would have a dust mass of 0.054 ME (4.4 ML). The disk also contains gas, as is indicated by the accretion of hydrogen, with the gas mass being on the order of 0.03 MJ (about 9.5 ME). ALMA did not detect any carbon monoxide in the disk.[2]

The SR 12 planetary system[2]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(years) 		Eccentricity Inclination Radius
c 11 ±3 MJ 980 — — — 1.6 RJ
  • Hubble image of SR 12 binary (upper right) and SR 12c (lower left). The orange part of the image shows H-alpha.
    Hubble image of SR 12 binary (upper right) and SR 12c (lower left). The orange part of the image shows H-alpha.
  • The binary SR 12 with Hubble
    The binary SR 12 with Hubble
  • Wide view around SR 12 with VISTA, showing many young stars in the Ophiuchus dark clouds. SR 12 is the blue star at the center and SR 12c is the faint blue "star" below SR 12.
    Wide view around SR 12 with VISTA, showing many young stars in the Ophiuchus dark clouds. SR 12 is the blue star at the center and SR 12c is the faint blue "star" below SR 12.

References

  1. ^ a b c Grankin, K. N.; Bouvier, J.; Herbst, W.; Melnikov, S. Yu. (2008-03-01). "Results of the ROTOR-program. II. The long-term photometric variability of weak-line T Tauri stars". Astronomy and Astrophysics. 479 (3): 827–843. arXiv:0801.3543. Bibcode:2008A&A...479..827G. doi:10.1051/0004-6361:20078476. ISSN 0004-6361.
  2. ^ a b c d e f g h i j k Wu, Ya-Lin; Bowler, Brendan P.; Sheehan, Patrick D.; Close, Laird M.; Eisner, Joshua A.; Best, William M. J.; Ward-Duong, Kimberly; Zhu, Zhaohuan; Kraus, Adam L. (2022-05-01). "ALMA Discovery of a Disk around the Planetary-mass Companion SR 12 c". The Astrophysical Journal. 930 (1): L3. arXiv:2204.06013. Bibcode:2022ApJ...930L...3W. doi:10.3847/2041-8213/ac6420. ISSN 0004-637X.
  3. ^ a b c d e Donati, J. -F.; Skelly, M. B.; Bouvier, J.; Jardine, M. M.; Gregory, S. G.; Morin, J.; Hussain, G. A. J.; Dougados, C.; Ménard, F.; Unruh, Y. (2010-03-01). "Complex magnetic topology and strong differential rotation on the low-mass T Tauri star V2247 Oph". Monthly Notices of the Royal Astronomical Society. 402 (3): 1426–1436. arXiv:0911.1080. Bibcode:2010MNRAS.402.1426D. doi:10.1111/j.1365-2966.2009.15998.x. ISSN 0035-8711.
  4. ^ Jönsson, Henrik; Holtzman, Jon A.; Allende Prieto, Carlos; Cunha, Katia; García-Hernández, D. A.; Hasselquist, Sten; Masseron, Thomas; Osorio, Yeisson; Shetrone, Matthew; Smith, Verne; Stringfellow, Guy S.; Bizyaev, Dmitry; Edvardsson, Bengt; Majewski, Steven R.; Mészáros, Szabolcs (2020-09-01). "APOGEE Data and Spectral Analysis from SDSS Data Release 16: Seven Years of Observations Including First Results from APOGEE-South". The Astronomical Journal. 160 (3): 120. arXiv:2007.05537. Bibcode:2020AJ....160..120J. doi:10.3847/1538-3881/aba592. ISSN 0004-6256.
  5. ^ a b 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.
  6. ^ a b c d Gras-Velázquez, À.; Ray, T. P. (2005-11-01). "Weak-line T Tauri stars: circumstellar disks and companions. I. Spectral energy distributions and infrared excesses". Astronomy and Astrophysics. 443 (2): 541–556. Bibcode:2005A&A...443..541G. doi:10.1051/0004-6361:20042397. ISSN 0004-6361.
  7. ^ a b Mason, Brian D.; Tokovinin, Andrei; Mendez, Rene A.; Costa, Edgardo (2023-10-01). "Speckle Interferometry at SOAR in 2022". The Astronomical Journal. 166 (4): 139. arXiv:2405.10071. Bibcode:2023AJ....166..139M. doi:10.3847/1538-3881/acedaf. ISSN 0004-6256.
  8. ^ Struve, Otto; Rudkjøbing, Mogens (1949-01-01). "Stellar Spectra with Emission Lines in the Obscuring Clouds of Ophiuchus and Scorpius". The Astrophysical Journal. 109: 92. Bibcode:1949ApJ...109...92S. doi:10.1086/145107. ISSN 0004-637X.
  9. ^ Montmerle, T.; Koch-Miramond, L.; Falgarone, E.; Grindlay, J. E. (1983-06-01). "Einstein observations of the Rho Ophiuchi dark cloud : an X-ray christmas tree". The Astrophysical Journal. 269: 182–201. Bibcode:1983ApJ...269..182M. doi:10.1086/161029. ISSN 0004-637X.
  10. ^ Simon, M.; Howell, R. R.; Longmore, A. J.; Wilking, B. A.; Peterson, D. M.; Chen, W. -P. (1987-09-01). "Milliarcsecond Resolution Infrared Observations of Young Stars in Taurus and Ophiuchus". The Astrophysical Journal. 320: 344. Bibcode:1987ApJ...320..344S. doi:10.1086/165548. ISSN 0004-637X.
  11. ^ Bouvier, J.; Appenzeller, I. (1992-02-01). "A magnitude-limited spectroscopic and photometric survey of rho OphiuchusX-ray sources". Astronomy and Astrophysics Supplement Series. 92: 481–516. Bibcode:1992A&AS...92..481B. ISSN 0365-0138.
  12. ^ a b c Kuzuhara, M.; Tamura, M.; Ishii, M.; Kudo, T.; Nishiyama, S.; Kandori, R. (2011-04-01). "The Widest-separation Substellar Companion Candidate to a Binary T Tauri Star". The Astronomical Journal. 141 (4): 119. Bibcode:2011AJ....141..119K. doi:10.1088/0004-6256/141/4/119. ISSN 0004-6256.
  13. ^ Allen, Lori E.; Myers, Philip C.; Di Francesco, James; Mathieu, Robert; Chen, Hua; Young, Erick (2002-02-01). "Hubble Space Telescope/NICMOS Imaging Survey of the Ophiuchus (Lynds 1688) Cluster". The Astrophysical Journal. 566 (2): 993–1004. arXiv:astro-ph/0110096. Bibcode:2002ApJ...566..993A. doi:10.1086/338128. ISSN 0004-637X.
  14. ^ Bowler, Brendan P.; Liu, Michael C.; Kraus, Adam L.; Mann, Andrew W. (2014-03-01). "Spectroscopic Confirmation of Young Planetary-mass Companions on Wide Orbits". The Astrophysical Journal. 784 (1): 65. arXiv:1401.7668. Bibcode:2014ApJ...784...65B. doi:10.1088/0004-637X/784/1/65. ISSN 0004-637X.
  15. ^ a b Santamaría-Miranda, Alejandro; Cáceres, Claudio; Schreiber, Matthias R.; Hardy, Adam; Bayo, Amelia; Parsons, Steven G.; Gromadzki, Mariusz; Aguayo Villegas, Aurora Belén (2018-04-01). "Accretion signatures in the X-shooter spectrum of the substellar companion to SR12". Monthly Notices of the Royal Astronomical Society. 475 (3): 2994–3003. arXiv:1712.09297. Bibcode:2018MNRAS.475.2994S. doi:10.1093/mnras/stx3325. ISSN 0035-8711.
  16. ^ Santamaría-Miranda, Alejandro; Cáceres, Claudio; Schreiber, Matthias R.; Hardy, Adam; Bayo, Amelia; Parsons, Steven G.; Gromadzki, Mariusz; Aguayo Villegas, Aurora Belén (2019-10-01). "Erratum: Accretion signatures in the X-shooter spectrum of the substellar companion to SR12". Monthly Notices of the Royal Astronomical Society. 488 (4): 5852–5853. Bibcode:2019MNRAS.488.5852S. doi:10.1093/mnras/stz2173. ISSN 0035-8711.
  17. ^ Martinez, Raquel A.; Kraus, Adam L. (2022-01-01). "A Mid-infrared Study of Directly Imaged Planetary-mass Companions Using Archival Spitzer/IRAC Images". The Astronomical Journal. 163 (1): 36. arXiv:2111.03087. Bibcode:2022AJ....163...36M. doi:10.3847/1538-3881/ac3745. ISSN 0004-6256.
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