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DS Tucanae

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DS Tucanae

DS Tucanae imaged with the NTT. DS Tucanae A is on the right and DS Tucanae B is on the left.
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Tucana
DS Tucanae A
Right ascension 23h 39m 39.48081s[1]
Declination −69° 11′ 44.7077″[1]
Apparent magnitude (V) 8.47[2]
DS Tucanae B
Right ascension 23h 39m 39.26965s[3]
Declination −69° 11′ 39.4936″[3]
Apparent magnitude (V) 9.84[4]
Characteristics
Spectral type G6V+K3V[4]
Variable type RS CVn[5]
Astrometry
A
Radial velocity (Rv)7.20[6] km/s
Proper motion (μ) RA: 79.529[1] mas/yr
Dec.: −67.551[1] mas/yr
Parallax (π)22.6367 ± 0.0150 mas[1]
Distance144.08 ± 0.10 ly
(44.18 ± 0.03 pc)
B
Radial velocity (Rv)5.32[7] km/s
Proper motion (μ) RA: 78.133[3] mas/yr
Dec.: −65.845[3] mas/yr
Parallax (π)22.6524 ± 0.0125 mas[3]
Distance143.98 ± 0.08 ly
(44.15 ± 0.02 pc)
Details
DS Tucanae A
Mass1.01±0.06[8] M☉
Radius0.964±0.029[8] R☉
Luminosity0.725±0.013[8] L☉
Temperature5,428±80[8] K
Rotational velocity (v sin i)27.75+1.73
−1.54[9] km/s
Age45±4[8] Myr
DS Tucanae B
Mass0.84±0.06[8] M☉
Radius0.864±0.036[8] R☉
Luminosity0.327±0.010[8] L☉
Temperature4,700±90[8] K
Age45±4[8] Myr
Other designations
DS Tuc, HD 222259, CCDM J23397-6912AB, CD−69°2106, HIP 116748, WDS J23397-6912AB, TIC 410214986, TOI 200
Database references
SIMBADAB
A
B
Ab

DS Tucanae (HD 222259) is a binary star system 144 light years away in the constellation of Tucana. It has an apparent visual magnitude of 8.5,[8] and is a RS Canum Venaticorum variable.[5] The system is notable for being young as a member of the 45 Myr old Tucana-Horologium moving group[10] and for the primary star hosting the confirmed exoplanet DS Tucanae Ab, discovered by THYME, using TESS.[11][8][12][13]

Stellar system

A light curve for DS Tucanae, plotted from TESS data[14]

DS Tucanae is a visual binary.[4] The binary consists of a G6V primary and a K3V secondary separated by 5″.[15] Based on radial velocity measurements it was suggested that the secondary itself is a binary, but later studies could not find evidence for this claim.[8]

Physical properties

High levels of magnetic activity, a strong 6708Å lithium line, and the position on the color-magnitude diagram, slightly above the main sequence, strongly support a young age of the system.[12] The primary star is emitting a frequent and powerful (up to 5-8×1034 ergs) X-ray flares.[16]

Both components of the binary are main sequence stars. The primary has a mass very similar to the Sun, but slightly cooler and smaller, meaning it is only 72% as luminous as the Sun. The secondary is only 84% as massive as the Sun and only 33% as luminous.

Planetary system

The DS Tuc A planetary system[8][12]
Companion
(in order from star) 		Mass Semimajor axis
(AU) 		Orbital period
(days) 		Eccentricity Inclination Radius
b <14.4[9] M🜨 0.18+0.13
−0.12 		8.138268 — 88.73+0.18
−0.17[9]° 		5.70±0.17 R🜨

DS Tuc Ab is one of the few transiting planets with an age smaller than 100 Myrs. Other examples are K2-33b, V1298 Tauri b and AU Microscopii b. Of these systems DS Tuc is the brightest and it is a good target for atmospheric characterization with JWST. The planet is a super-Neptune or sub-Saturn.[8] The planet might be an inflated planet with an upper mass limit of 20 ME.[12] DS Tuc Ab will be observed by ESA's CHEOPS mission to characterize the planet.[17]

The planet DS Tucanae Ab has a low orbital obliquity (λ = 2.93°+0.88°
−0.87° or λ = 12°±13°). This means that the orbital plane of this planet aligns with the stellar equator of the star. This is unusual for a short period planet. Many short period planets show high orbital obliquity, which was taken as a sign of the scattering of the planet into this short period orbit. It can also be interpreted as the formation of a planet in an inner disk with an axial tilt. But these previous measurements of orbital obliquity were made for giant planets around mature stars. DS Tucanae Ab is a relatively small young planet. This suggests that DS Tucanae Ab formed in a smooth disk that was not perturbed by the stellar companion DS Tucanae B.[18][19] DS Tucanae Ab might therefore be a good target to study in-situ planet-formation of short-period planets.

References

  1. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ^ Høg, E.; Fabricius, C.; Makarov, V. V.; Urban, S.; Corbin, T.; Wycoff, G.; Bastian, U.; Schwekendiek, P.; Wicenec, A. (March 2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics. 355: L27–L30. Bibcode:2000A&A...355L..27H. ISSN 0004-6361.
  3. ^ a b c d e Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics. 649: A1. arXiv:2012.01533. Bibcode:2021A&A...649A...1G. doi:10.1051/0004-6361/202039657. S2CID 227254300. (Erratum: doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  4. ^ a b c Torres, G. (August 1988). "Visual Measurements of Southern Double Stars - Part Three". Astrophysics and Space Science. 147 (2): 257–266. Bibcode:1988Ap&SS.147..257T. doi:10.1007/BF00645670. ISSN 0004-640X. S2CID 116982206.
  5. ^ a b Samus', N. N.; Goranskii, V. P.; Durlevich, O. V.; Zharova, A. V.; Kazarovets, E. V.; Kireeva, N. N.; Pastukhova, E. N.; Williams, D. B.; Hazen, M. L. (July 2003). "An Electronic Version of the Second Volume of the General Catalogue of Variable Stars with Improved Coordinates". Astronomy Letters. 29 (7): 468–479. Bibcode:2003AstL...29..468S. doi:10.1134/1.1589864. ISSN 1063-7737. S2CID 16299532.
  6. ^ 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.
  7. ^ 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.
  8. ^ a b c d e f g h i j k l m n o Newton, Elisabeth R.; et al. (July 2019). "TESS Hunt for Young and Maturing Exoplanets (THYME): A Planet in the 45 Myr Tucana-Horologium Association". The Astrophysical Journal Letters. 880 (1): L17. arXiv:1906.10703. Bibcode:2019ApJ...880L..17N. doi:10.3847/2041-8213/ab2988. hdl:1721.1/124722. ISSN 0004-637X. S2CID 195658207.
  9. ^ a b c Benatti, S.; Damasso, M.; Borsa, F.; Locci, D.; Pillitteri, I.; Desidera, S.; Maggio, A.; Micela, G.; Wolk, S.; Claudi, R.; Malavolta, L.; Modirrousta-Galian, D. (2021), "Constraints on the mass and on the atmospheric composition and evolution of the low-density young planet DS Tucanae a B", Astronomy & Astrophysics, 650: A66, arXiv:2103.12922, Bibcode:2021A&A...650A..66B, doi:10.1051/0004-6361/202140416, S2CID 234864890
  10. ^ Zuckerman, B.; Webb, R. A. (2000-06-01). "Identification of a Nearby Stellar Association in theHipparcos Catalog: Implications for Recent, Local Star Formation". The Astrophysical Journal. 535 (2): 959. arXiv:astro-ph/0002461. Bibcode:2000ApJ...535..959Z. doi:10.1086/308897. ISSN 0004-637X. S2CID 2485534.
  11. ^ Albright, Charlotte (14 August 2019). "Dartmouth Astronomer on Leading Discovery of a New Planet | Dartmouth News". news.dartmouth.edu. Retrieved 2022-01-30.
  12. ^ a b c d Benatti, S.; Nardiello, D.; Malavolta, L.; Desidera, S.; Borsato, L.; Nascimbeni, V.; Damasso, M.; D'Orazi, V.; Mesa, D.; Messina, S.; Esposito, M.; Bignamini, A.; Claudi, R.; Covino, E.; Lovis, C.; Sabotta, S. (October 2019). "A possibly inflated planet around the bright young star DS Tucanae A". Astronomy & Astrophysics. 630: A81. arXiv:1904.01591. Bibcode:2019A&A...630A..81B. doi:10.1051/0004-6361/201935598. ISSN 0004-6361. S2CID 102486551.
  13. ^ "DS Tuc A b". exoplanetarchive.ipac.caltech.edu. Retrieved 2019-12-18.
  14. ^ "MAST: Barbara A. Mikulski Archive for Space Telescopes". Space Telescope Science Institute. Retrieved 8 December 2021.
  15. ^ Torres, C. a. O.; Quast, G. R.; Silva, L. da; Reza, R. de la; Melo, C. H. F.; Sterzik, M. (2006-12-01). "Search for associations containing young stars (SACY) - I. Sample and searching method". Astronomy & Astrophysics. 460 (3): 695–708. arXiv:astro-ph/0609258. Bibcode:2006A&A...460..695T. doi:10.1051/0004-6361:20065602. ISSN 0004-6361. S2CID 16080025.
  16. ^ Pillitteri, I.; Argiroffi, C.; Maggio, A.; Micela, G.; Benatti, S.; Reale, F.; Colombo, S.; Wolk, S. J. (2022), "X-ray flares of the young planet host Ds Tucanae A", Astronomy & Astrophysics, 666: A198, arXiv:2208.07415, Bibcode:2022A&A...666A.198P, doi:10.1051/0004-6361/202244268, S2CID 251589568
  17. ^ "AO-1 Programmes - CHEOPS Guest Observers Programme - Cosmos". www.cosmos.esa.int. Retrieved 2019-12-18.
  18. ^ Montet, Benjamin T.; Feinstein, Adina D.; Luger, Rodrigo; Bedell, Megan E.; Gully-Santiago, Michael A.; Teske, Johanna K.; Xuesong Wang, Sharon; Butler, R. Paul; Flowers, Erin; Shectman, Stephen A.; Crane, Jeffrey D. (2020). "The Young Planet DS Tuc Ab has a Low Obliquity". The Astronomical Journal. 159 (3): 112. arXiv:1912.03794. Bibcode:2020AJ....159..112M. doi:10.3847/1538-3881/ab6d6d. S2CID 208920990.
  19. ^ Zhou, G.; Winn, J. N.; Newton, E. R.; Quinn, S. N.; Rodriguez, J. E.; Mann, A. W.; Rizzuto, A. C.; Vanderburg, A. M.; Huang, C. X.; Latham, D. W.; Teske, J. K. (2020). "A well aligned orbit for the 45 Myr old transiting Neptune DS Tuc Ab". The Astrophysical Journal. 892 (2): L21. arXiv:1912.04095. Bibcode:2020ApJ...892L..21Z. doi:10.3847/2041-8213/ab7d3c. S2CID 208910672.
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