Sökning: WFRF:(Persson B.) > The young HD 73583 ...
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000 | 11341naa a2201657 4500 | |
001 | oai:research.chalmers.se:186f1b0e-3b02-4788-bd60-ba2b4dc427be | |
003 | SwePub | |
008 | 220623s2022 | |||||||||||000 ||eng| | |
024 | 7 | a https://research.chalmers.se/publication/5309032 URI |
024 | 7 | a https://doi.org/10.1093/mnras/stac6382 DOI |
040 | a (SwePub)cth | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a art2 swepub-publicationtype |
072 | 7 | a ref2 swepub-contenttype |
100 | 1 | a Barragan, O.u University Of Oxford4 aut |
245 | 1 0 | a The young HD 73583 (TOI-560) planetary system: two 10-M-circle plus mini-Neptunes transiting a 500-Myr-old, bright, and active K dwarf |
264 | c 2022-03-15 | |
264 | 1 | b Oxford University Press (OUP),c 2022 |
338 | a electronic2 rdacarrier | |
520 | a We present the discovery and characterization of two transiting planets observed by TESS in the light curves of the young and bright (V = 9.67) star HD73583 (TOI-560). We perform an intensive spectroscopic and photometric space- and ground-based follow-up in order to confirm and characterize the system. We found that HD73583 is a young (similar to 500 Myr) active star with a rotational period of 12.08 +/- 0.11 d, and a mass and radius of 0.73 +/- 0.02 M-circle dot and 0.65 +/- 0.02 R-circle dot, respectively. HD 73583 b (P-b = 6.3980420(-0.0000062)(+0.0000067 )d) has a mass and radius of 10.2(-3.1)(+3.4) M-circle plus and 2.79 +/- 0.10 R-circle plus, respectively, which gives a density of 2.58(-0.81)(+0.95) g cm(-3). HD 73583 c (P-c = 18.87974(-0.00074)(+0.00086) d) has a mass and radius of 9.7(-1.7)(+1.8) M-circle plus and 2.39(-0.09)(+0.10) R-circle plus, respectively, which translates to a density of 3.88(-0.80)(+0.91) g cm(-3). Both planets are consistent with worlds made of a solid core surrounded by a volatile envelope. Because of their youth and host star brightness, they both are excellent candidates to perform transmission spectroscopy studies. We expect ongoing atmospheric mass-loss for both planets caused by stellar irradiation. We estimate that the detection of evaporating signatures on H and He would be challenging, but doable with present and future instruments. | |
650 | 7 | a NATURVETENSKAPx Fysikx Subatomär fysik0 (SwePub)103012 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Subatomic Physics0 (SwePub)103012 hsv//eng |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
650 | 7 | a NATURVETENSKAPx Fysikx Annan fysik0 (SwePub)103992 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Other Physics Topics0 (SwePub)103992 hsv//eng |
653 | a techniques: radial velocities | |
653 | a stars: activity | |
653 | a planets and satellites: individual: HD 73583 (TOI-560) | |
653 | a techniques: photometric | |
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700 | 1 | a Smith, A. M. S.u University Of Leicester4 aut |
700 | 1 | a Subjak, J.u Univerzita Karlova,Charles University,Czech Academy of Sciences4 aut |
700 | 1 | a Tan, T. G.u Curtin University4 aut |
700 | 1 | a Udry, S.u Université de Genève,University of Geneva4 aut |
700 | 1 | a Watson, C.u Queen's University Belfast4 aut |
700 | 1 | a Wheatley, P. J.u The University of Warwick4 aut |
700 | 1 | a West, R.u The University of Warwick4 aut |
700 | 1 | a Winn, J. N.u Princeton University4 aut |
700 | 1 | a Wang, S. X.u Tsinghua University4 aut |
700 | 1 | a Wolfgang, A.4 aut |
700 | 1 | a Ziegler, C.u Stephen F. Austin State University4 aut |
710 | 2 | a University Of Oxfordb The University of Warwick4 org |
773 | 0 | t Monthly Notices of the Royal Astronomical Societyd : Oxford University Press (OUP)g 514:2, s. 1606-1627q 514:2<1606-1627x 0035-8711x 1365-2966 |
856 | 4 | u https://research.chalmers.se/publication/530903/file/530903_Fulltext.pdfx primaryx freey FULLTEXT |
856 | 4 8 | u https://research.chalmers.se/publication/530903 |
856 | 4 8 | u https://doi.org/10.1093/mnras/stac638 |
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