Astronomy:HD 131399
File:SPHERE observations of the planet HD 131399Ab.tif SPHERE image of HD 131399 A (top left), B and C (bottom right), and the background object (center) Credit: ESO/K. Wagner et al. | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Centaurus |
| Right ascension | 14h 54m 25.30919s[1] |
| Declination | −34° 08′ 34.0412″[1] |
| Apparent magnitude (V) | 7.07[2] |
| Characteristics | |
| Spectral type | A1V + G + K[3] |
| Astrometry | |
| Radial velocity (Rv) | 0.30 ± 1.3[4] km/s |
| Distance | 351+15 −12 ly (107.9+4.5 −3.7[5] pc) |
| A | |
| Proper motion (μ) | RA: −30.702[6] mas/yr Dec.: −30.774[6] mas/yr |
| Parallax (π) | 9.7480 ± 0.0357[6] mas |
| Distance | 335 ± 1 ly (102.6 ± 0.4 pc) |
| Absolute magnitude (MV) | 1.89[7] |
| BC | |
| Proper motion (μ) | RA: −31.523[8] mas/yr Dec.: −31.047[8] mas/yr |
| Parallax (π) | 9.3021 ± 0.0633[8] mas |
| Distance | 351 ± 2 ly (107.5 ± 0.7 pc) |
| Orbit[3] | |
| Primary | A |
| Companion | BC |
| Period (P) | 3556 ± 36 yr |
| Semi-major axis (a) | 3.56 ± 0.03″ (349 ± 28 au) |
| Eccentricity (e) | 0.13 ± 0.05 |
| Inclination (i) | 45 to 65° |
| Longitude of the node (Ω) | 265 ± 20[note 1]° |
| Periastron epoch (T) | B 502 ± 33 |
| Argument of periastron (ω) (secondary) | 145.3 ± 15[note 2]° |
| Details | |
| Age | 21.9+4.1 −3.8[5] Myr |
| HD 131399 A | |
| Mass | 1.95+0.08 −0.06[7] M☉ |
| Radius | 1.51+0.13 −0.10[7] R☉ |
| Luminosity | 14.8+2.6 −2.2[7] L☉ |
| Surface gravity (log g) | 4.37±0.10[7] cgs |
| Temperature | 9,200±100[7] K |
| Rotational velocity (v sin i) | 26±2[7] km/s |
| HD 131399 B | |
| Mass | 0.95±0.04[5] M☉ |
| Surface gravity (log g) | 4.40±0.03[5] cgs |
| Temperature | 4,890+190 −170[5] K |
| HD 131399 C | |
| Mass | 0.35±0.04[5] M☉ |
| Surface gravity (log g) | 4.45±0.05[5] cgs |
| Temperature | 3,460±60[5] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
HD 131399 is a star system in the constellation of Centaurus. Based on the system's electromagnetic spectrum, it is located around 350 light-years (107.9 parsecs) away.[5] The total apparent magnitude is 7.07,[5] but because of interstellar dust between it and the Earth, it appears 0.22 ± 0.09 magnitudes dimmer than it should be.[5]
The brightest star, is a young A-type main-sequence star, and further out are two lower-mass stars.[3] A Jupiter-mass planet or a low-mass brown dwarf was once thought to be orbiting the central star, but this has been ruled out.[5][9]
Stellar system
The brightest star in the HD 131399 system is designated HD 131399 A. Its spectral type is A1V,[3] and it is 2.08 times as massive as the Sun.[5] The two lower-mass stars are designated HD 131399 B and C, respectively. B is a G-type main-sequence star, while HD 131399 C is a K-type main-sequence star.[3] Both stars are less massive than the Sun.[5]
HD 131399 B and C are located very close to each other, and the two orbit each other at about 10 AU.[10] In turn, the B-C pair orbits the central star A at a distance of 349 astronomical units (au). This orbit takes about 3,600 years to complete, and it has an eccentricity of about 0.13[3] The entire system is about 21.9 million years old.[5]
One paper has reported that HD 131399 A has a companion in an inclined 10-day orbit with a semi-major axis of 0.1 astronomical unit|AU.[11] HD 131399 A has been described as a "nascent Am star"; although it has a very slow projected rotation rate and would be expected to show chemical peculiarities, its spectrum is relatively normal, possibly due to its young age.[7]
Planetary system
File:An artist’s impression of planet in the HD 131399 system.tif The claimed discovery of a massive planet, named HD 131399 Ab, was announced in a paper published in the journal Science.[3] The object was imaged using the SPHERE imager of the Very Large Telescope at the European Southern Observatory, located in the Atacama Desert of Chile , and announced in a July 2016 paper in the journal Science.[3][12] It was thought to be a T-type object with a mass of 4 ± 1 MJ,[3] but its orbit would have been unstable, causing it to be ejected between the primary's red giant phase and white dwarf phase.[13] This was the first exoplanet candidate to be discovered by SPHERE. The image was created from two separate SPHERE observations: one to image the three stars and one to detect the faint planet.[14] After its discovery, the team unofficially named the system "Scorpion-1" and the planet "Scorpion-1b", after the survey that prompted its discovery, the Scorpion Planet Survey (principal investigator: Daniel Apai).[15]
In May 2017, observations made by the Gemini Planet Imager and including a reanalysis of the SPHERE data suggest that this target is, in fact, a background star. This object's spectrum seems to be like that of a K-type or M-type dwarf, not a T-type object as first thought. It also initially appeared to be associated with HD 131399, but this was because of its unusually high proper motion (in the top 4% fastest-moving stars).[5] After subsequent data published in 2022 confirmed that the object is a background star, the paper announcing the putative discovery was retracted.[9][16]
Characteristics
The planet was thought to be about 16 million years old, with a mass of 4 (± 1) MJ (Jupiter masses), and a temperature of 850 K (577 °C; 1,070 °F) (± 50 K), which would make it one of the coldest and least massive directly imaged exoplanets.[10] Its atmosphere was shown to contain both water and methane through the use of near-infrared spectroscopy (1.4-1.6 μm).[3] Scientists believed it was unlikely that the planet harbored life due to it being gaseous. The planet was said to have "no liquid water, extremely powerful winds, and no surface; just below the uppermost layer of the atmosphere it rains liquid iron droplets."[17] One orbit of HD 131399 Ab was thought to take 550 years.[3][12]
References
- ↑ 1.0 1.1 van Leeuwen, F. (2007). "Validation of the new Hipparcos reduction". Astronomy and Astrophysics 474 (2): 653–664. doi:10.1051/0004-6361:20078357. Bibcode: 2007A&A...474..653V. http://www.aanda.org/index.php?option=com_article&access=bibcode&Itemid=129&bibcode=2007A%2526A...474..653VFUL.
- ↑ Høg, E. (2000). "The Tycho-2 catalogue of the 2.5 million brightest stars". Astronomy and Astrophysics 355: L27–L30. Bibcode: 2000A&A...355L..27H.
- ↑ 3.00 3.01 3.02 3.03 3.04 3.05 3.06 3.07 3.08 3.09 3.10 Wagner, K.; Apai, D.; Kasper, M.; Kratter, K.; McClure, M.; Robberto, M.; Beuzit, J.-L. (2016). "Direct imaging discovery of a Jovian exoplanet within a triple-star system". Science 353 (6300): 673–8. doi:10.1126/science.aaf9671. PMID 27386921. Bibcode: 2016Sci...353..673W. (Retracted, see doi:10.1126/science.abq1709)
- ↑ Kharchenko, N. V. (2007). "Astrophysical supplements to the ASCC-2.5: Ia. Radial velocities of ~55000 stars and mean radial velocities of 516 Galactic open clusters and associations". Astronomische Nachrichten 328 (9): 889. doi:10.1002/asna.200710776. Bibcode: 2007AN....328..889K.
- ↑ 5.00 5.01 5.02 5.03 5.04 5.05 5.06 5.07 5.08 5.09 5.10 5.11 5.12 5.13 5.14 5.15 Nielsen, Eric L. (2017). "Evidence that the Directly-Imaged Planet HD 131399 Ab is a Background Star". The Astronomical Journal 154 (6): 218. doi:10.3847/1538-3881/aa8a69. Bibcode: 2017AJ....154..218N.
- ↑ 6.0 6.1 6.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 7.0 7.1 7.2 7.3 7.4 7.5 7.6 7.7 Przybilla, N.; Aschenbrenner, P.; Buder, S. (2017). "Candidate exoplanet host HD 131399A: A nascent Am star". Astronomy & Astrophysics 604: L9. doi:10.1051/0004-6361/201731384. Bibcode: 2017A&A...604L...9P.
- ↑ 8.0 8.1 8.2 Brown, A. G. A. (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics 649: A1. doi:10.1051/0004-6361/202039657. Bibcode: 2021A&A...649A...1G. Gaia EDR3 record for this source at VizieR.
- ↑ 9.0 9.1 Wagner, Kevin; Apai, Dániel; Kasper, Markus; Kratter, Kaitlin; McClure, Melissa; Robberto, Massimo; Beuzit, Jean-Luc (2022-04-15). "Retraction" (in en). Science 376 (6590): 255. doi:10.1126/science.abq1709. ISSN 0036-8075. PMID 35420970. Bibcode: 2022Sci...376..255W. https://www.science.org/doi/10.1126/science.abq1709.
- ↑ 10.0 10.1 "HD 131399Ab: Astronomers Find Super-Jupiter in Triple-Star System | Astronomy | Sci-News.com" (in en-US). http://www.sci-news.com/astronomy/hd-131399ab-super-jupiter-triple-star-system-04008.html.
- ↑ Lagrange, A.-M.; Keppler, M.; Beust, H.; Rodet, L.; Meunier, N.; Lillo-Box, J.; Bonnefoy, M.; Galland, F. (2017). "Discovery of a stellar companion to HD 131399A". Astronomy & Astrophysics 608: L9. doi:10.1051/0004-6361/201730978. Bibcode: 2017A&A...608L...9L.
- ↑ 12.0 12.1 "This strange new planet has three suns". CBS News. 7 July 2016. https://www.cbsnews.com/news/planet-with-three-suns-triple-sunrises-sunsets/.
- ↑ Veras, Dimitri; Mustill, Alexander J.; Gänsicke, Boris T. (2017). "The unstable fate of the planet orbiting the a star in the HD 131399 triple stellar system". Monthly Notices of the Royal Astronomical Society 465 (2): 1499. doi:10.1093/mnras/stw2821. Bibcode: 2017MNRAS.465.1499V.
- ↑ "A Surprising Planet with Three Suns". ESO. https://www.eso.org/public/news/eso1624/.
- ↑ Miller, Michael (12 April 2017). "UC mountaineer, galactic explorer". University of Cincinnati. http://magazine.uc.edu/editors_picks/recent_features/scorpion.html.
- ↑ Oransky, Ivan (14 April 2022). "Triple sunrise, triple sunset: Science paper retracted when it turns out a planet is a star". https://retractionwatch.com/2022/04/14/triple-sunrise-triple-sunset-science-paper-retracted-when-it-turns-out-a-planet-is-a-star/#more-124683.
- ↑ "16-million-year-old planet with three suns discovered". MSN. 8 July 2016. https://www.msn.com/en-gb/news/techandscience/16-million-year-old-planet-with-three-suns-discovered/ar-BBu52Bi?li=BBoPOOl.
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