2024A&A...690A.349N

Query : 2024A&A...690A.349N

2024A&A...690A.349N - Astronomy and Astrophysics, volume 690A349 (2024/10-1)

The K2-24 planetary system revisited by CHEOPS.

NASCIMBENI V., BORSATO L., LEONARDI P., SOUSA S.G., WILSON T.G., FORTIER A., HEITZMANN A., MANTOVAN G., LUQUE R., ZINGALES T., PIOTTO G., ALIBERT Y., ALONSO R., BARCZY T., BARRADO NAVASCUES D., BARROS S.C.C., BAUMJOHANN W., BECK T., BENZ W., BILLOT N., BIONDI F., BRANDEKER A., BROEG C., BUSCH M.-D., COLLIER CAMERON A., CORREIA A.C.M., CSIZMADIA S., CUBILLOS P.E., DAVIES M.B., DELEUIL M., DELINE A., DELREZ L., DEMANGEON O.D.S., DEMORY B.-O., DEREKAS A., EDWARDS B., EHRENREICH D., ERIKSON A., FOSSATI L., FRIDLUND M., GANDOLFI D., GAZEAS K., GILLON M., GUDEL M., GUNTHER M.N., HELLING C., ISAAK K.G., KERSCHBAUM F., KISS L.L., KORTH J., LAM K.W.F., LASKAR J., LECAVELIER DES ETANGS A., LELEU A., LENDL M., MAGRIN D., MAXTED P.F.L., MERIN B., MORDASINI C., OLOFSSON G., OTTENSAMER R., PAGANO I., PALLE E., PETER G., POLLACCO D., QUELOZ D., RAGAZZONI R., RANDO N., RAUER H., RIBAS I., SANTOS N.C., SCANDARIATO G., SEGRANSAN D., SIMON A.E., SMITH A.M.S., SOUTHWORTH R., STALPORT M., SULIS S., SZABO G.M., UDRY S., ULMER B., VAN GROOTEL V., VENTURINI J., VILLAVER E. and WALTON N.A.

Abstract (from CDS):

The planetary system K2-24 is composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large transit time variations (TTVs), and it is an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer, and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the scenario of pure disk migration through resonant capture. With 13 new CHEOPS light curves (seven of planet b, six of planet c), we carried out a global photometric and dynamical re-analysis by including all the available literature data as well. We obtained the most accurate set of planetary parameters to date for the K2-24 system, including radii and masses at 1% and 5% precision (now essentially limited by the uncertainty on stellar parameters) and non-zero eccentricities eb = 0.0498–0.0018+0.0011, ec = 0.0282–0.0007+0.0003 detected at very high significance for both planets. Such relatively large values imply the need for an additional physical mechanism of eccentricity excitation during or after the migration stage. Also, while the accuracy of the previous TTV model had drifted by up to 0.5 days at the current time, we constrained the orbital solution firmly enough to predict the forthcoming transits for the next ∼15 years, thus enabling efficient follow-up with top-level facilities such as JWST or ESPRESSO.

Abstract Copyright: © The Authors 2024

Journal keyword(s): techniques: photometric - techniques: spectroscopic - planets and satellites: detection - planets and satellites: dynamical evolution and stability - planets and satellites: gaseous planets

VizieR on-line data: <Available at CDS (J/A+A/690/A349): table3.dat lcs.dat predtt.dat>

Simbad objects: 28

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Number of rows : 28
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 TYC 5881-551-1 * 03 50 37.7059031328 -15 01 33.997997424   12.83 11.94     ~ 10 0
2 TOI-216 PM* 04 55 55.2548838048 -63 15 36.313162056           ~ 58 0
3 TOI-2525c Pl 05 47 24.1880042543 -60 31 17.070197468           ~ 7 0
4 TOI-2525b Pl 05 47 24.1880042543 -60 31 17.070197468           ~ 12 0
5 K2-146b Pl 08 40 06.4242250368 +19 05 34.430759088           ~ 29 0
6 K2-146c Pl 08 40 06.4242250368 +19 05 34.430759088           ~ 22 0
7 K2-146 LM* 08 40 06.4242250368 +19 05 34.430759088   17.87 16.25 15.97   M3.0V 49 0
8 K2-19 * 11 39 50.4803341248 +00 36 12.875047920   13.80 13.00 12.88   G7 75 0
9 K2-19b Pl 11 39 50.4803341248 +00 36 12.875047920           ~ 42 0
10 K2-19c Pl 11 39 50.4803341248 +00 36 12.875047920           ~ 41 0
11 CD-24 12581 PM* 16 10 17.6976776832 -24 59 25.260709632   12.22 11.28     ~ 58 0
12 CD-24 12581c Pl 16 10 17.6976776832 -24 59 25.260709632           ~ 39 0
13 CD-24 12581d Pl 16 10 17.6976776832 -24 59 25.260709632           ~ 4 0
14 CD-24 12581b Pl 16 10 17.6976776832 -24 59 25.260709632           ~ 45 0
15 Kepler-30b Pl 19 01 08.0746104528 +38 56 50.218268856           ~ 89 1
16 Kepler-30c Pl 19 01 08.0746104528 +38 56 50.218268856           ~ 78 1
17 Kepler-9 Er* 19 02 17.7544327200 +38 24 03.176851896     13.9 13.791   G2 223 1
18 Kepler-9c Pl 19 02 17.7544327200 +38 24 03.176851896           ~ 109 1
19 Kepler-9b Pl 19 02 17.7544327200 +38 24 03.176851896           ~ 121 1
20 Kepler-1972 Ro* 19 13 34.8691439904 +39 52 21.469843704   11.8 11.2     ~ 34 0
21 Kepler-88c Pl 19 24 35.5430965488 +40 40 09.809893020           ~ 23 1
22 Kepler-88b Pl 19 24 35.5430965488 +40 40 09.809893020           ~ 68 1
23 Kepler-88 Er* 19 24 35.5430965488 +40 40 09.809893020   14.192 13.257 13.084   G8IV 101 1
24 Kepler-223b Pl 19 53 16.4202435936 +47 16 46.308434088           ~ 37 0
25 Kepler-223 Er* 19 53 16.4202435936 +47 16 46.308434088   16.209 15.570 15.78   ~ 192 1
26 Kepler-223c Pl 19 53 16.4202435936 +47 16 46.308434088           ~ 37 0
27 Kepler-1705 Ro* 20 06 18.8492915448 +44 18 43.833260880           ~ 21 0
28 WASP-47 * 22 04 48.7261549272 -12 01 07.998743676     11.99 11.82   ~ 217 1

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