Das Tautenburg-Ondrejov Radialgeschwindigkeitsprogamm bedeckender Planeten von Sternen unterschiedlicher Masse
Zusammenfassung der Projektergebnisse
In the last decade it became clear that the diversity of exoplanets is much larger than those of planets in our solar system. This large diversity must be related to the formation and early evolution of the planets and in particular the properties of the disk from which these planets formed. Since the masses and the lifetime of the disks depend on the mass of star, it is expected that properties of the planets also depend on the mass of the host star. In other words, it is expected that the occurrence rate and masses of the planets that depends on the mass of the host star. The result of this study is that this is in fact the case. Because planets of solar-like stars have already been studied in detail, we focused in our study on two samples of stars: One sample has significantly higher masses than our sun (intermediate-mass stars), and the other one contains stars that have much lower masses than our sun (M-stars). Prior to our study, it had been claimed that intermediate-mass stars have a very high occurrence rate of close-in massive planets. We ruled out this possibility, and showed that the occurrence rate of close-in, massive planets for intermediate-mass stars is 0.75%, or lower. This is comparable or even lower than that of solar-like stars. Massive planets of low-mass stars exist but are extremely rare. In contrast to this, the occurrence rate of planet in the mass-range between one MEarth and ten MEarth with periods up to 100 days orbiting low-mass stars is high. In other words, high-mass planets of low-mass stars are rare but the occurrence rate for planets which have less than 10 MEarth is at least a factor two higher than that for solar like stars. We thus conclude that the properties of planets strongly depend on the mass of the host star.
Projektbezogene Publikationen (Auswahl)
- 2021. The CARMENES search for exoplanets around M dwarfs - Planet occurrence rates from a subsample of 71 stars
Sabotta S., Schlecker M., Chaturvedi P., Guenther E.W., Muñoz Rodríguez I., Muñoz Sánchez J.C., Caballero J.A., et al.
(Siehe online unter https://doi.org/10.48550/arXiv.2107.03802) - 2017, A&A, 608, A93. K2-106, a system containing a metal-rich planet and a planet of lower density
Guenther E.W., Barragán O., Dai F., Gandolfi D., Hirano T., Fridlund M., Fossati L., et al.
(Siehe online unter https://doi.org/10.1051/0004-6361/201730885) - 2019, MNRAS, 487, 4230: HD 99458: First time ever Ap-type star as a δ Scuti pulsator in a short period eclipsing binary?
Skarka M., Kabáth P., Paunzen E., Fedurco M., Budaj J., Dupkala D., Krtivka J., et al.
(Siehe online unter https://doi.org/10.1093/mnras/stz1478) - 2019, MNRAS, 489, 2069: Lack of close-in, massive planets of main-sequence A-type stars from Kepler
Sabotta S., Kabáth P., Korth J., Guenther E.W., Dupkala D., Grziwa S., Klocova T., et al.
(Siehe online unter https://doi.org/10.1093/mnras/stz2232) - 2020, PASP, 132, 035002: Ondřejov Echelle Spectrograph, Ground Based Support Facility for Exoplanet Missions
Kabáth P., Skarka M., Sabotta S., Guenther E., Jones D., Klocová T., Subjak J., et al.
(Siehe online unter https://doi.org/10.1088/1538-3873/ab6752)
