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Obliquities of exoplanet host stars: Nineteen new and updated measurements, and trends in the sample of 205 measurements

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Title: Obliquities of exoplanet host stars: Nineteen new and updated measurements, and trends in the sample of 205 measurements
Authors: Knudstrup, Emil, 1990, Albrecht, Simon, Winn, J. N., Gandolfi, D., Zanazzi, J. J., Persson, Carina, 1964, Fridlund, Malcolm, 1952, Marcussen, M. L., Chontos, A., Keniger, Marcelo Aron Fetzner, Eisner, N. L., Bieryla, Allyson, Isaacson, H., Howard, A. W., Hirsch, L.A., Murgas, F., Narita, Norio, Palle, Enric, Kawai, Yugo, Baker, D.
Source: Exoplaneter från rymden - CHEOPS och PLATO, ESA's nästa två rymdteleskop (fas 2) Astronomy and Astrophysics Additional tables: Obliquities of exoplanet host stars. Nineteen new, updated measurements for the sample of 205 measurements and observed trends. 690
Subject Terms: Planet-star interactions, Planets and satellites: dynamical evolution and stability, Planets and satellites: formation
Description: Measurements of the obliquities in exoplanet systems have revealed some remarkable architectures, some of which are very different from the Solar System. Nearly 200 obliquity measurements have been obtained through observations of the Rossiter McLaughlin (RM) effect. Here, we report on observations of 19 planetary systems that led to 17 clear detections of the RM effect and 2 less secure detections. After adding the new measurements to the tally, we used the entire collection of RM measurements to investigate four issues that have arisen in the literature. i) Does the obliquity distribution show a peak at approximately 90 ? We find tentative evidence that such a peak does exist when restricting attention to the sample of sub-Saturn planets and hot Jupiters orbiting F stars. ii) Are high obliquities associated with high eccentricities? We find the association to be weaker than previously reported, and that a stronger association exists between obliquity and orbital separation, possibly due to tidal obliquity damping at small separations. iii) How low are the lowest known obliquities? Among hot Jupiters around cool stars, we find the dispersion to be 1.4 ± 0.7, smaller than the 6 obliquity of the Sun, which serves as additional evidence for tidal damping. iv) What are the obliquities of stars with compact and flat systems of multiple planets? We find that they generally have obliquities lower than 10, with several remarkable exceptions possibly caused by wide-orbiting stellar or planetary companions.
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  Data: Obliquities of exoplanet host stars: Nineteen new and updated measurements, and trends in the sample of 205 measurements
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  Data: <searchLink fieldCode="AR" term="%22Knudstrup%2C+Emil%22">Knudstrup, Emil</searchLink>, 1990<br /><searchLink fieldCode="AR" term="%22Albrecht%2C+Simon%22">Albrecht, Simon</searchLink><br /><searchLink fieldCode="AR" term="%22Winn%2C+J%2E+N%2E%22">Winn, J. N.</searchLink><br /><searchLink fieldCode="AR" term="%22Gandolfi%2C+D%2E%22">Gandolfi, D.</searchLink><br /><searchLink fieldCode="AR" term="%22Zanazzi%2C+J%2E+J%2E%22">Zanazzi, J. J.</searchLink><br /><searchLink fieldCode="AR" term="%22Persson%2C+Carina%22">Persson, Carina</searchLink>, 1964<br /><searchLink fieldCode="AR" term="%22Fridlund%2C+Malcolm%22">Fridlund, Malcolm</searchLink>, 1952<br /><searchLink fieldCode="AR" term="%22Marcussen%2C+M%2E+L%2E%22">Marcussen, M. L.</searchLink><br /><searchLink fieldCode="AR" term="%22Chontos%2C+A%2E%22">Chontos, A.</searchLink><br /><searchLink fieldCode="AR" term="%22Keniger%2C+Marcelo+Aron+Fetzner%22">Keniger, Marcelo Aron Fetzner</searchLink><br /><searchLink fieldCode="AR" term="%22Eisner%2C+N%2E+L%2E%22">Eisner, N. L.</searchLink><br /><searchLink fieldCode="AR" term="%22Bieryla%2C+Allyson%22">Bieryla, Allyson</searchLink><br /><searchLink fieldCode="AR" term="%22Isaacson%2C+H%2E%22">Isaacson, H.</searchLink><br /><searchLink fieldCode="AR" term="%22Howard%2C+A%2E+W%2E%22">Howard, A. W.</searchLink><br /><searchLink fieldCode="AR" term="%22Hirsch%2C+L%2EA%2E%22">Hirsch, L.A.</searchLink><br /><searchLink fieldCode="AR" term="%22Murgas%2C+F%2E%22">Murgas, F.</searchLink><br /><searchLink fieldCode="AR" term="%22Narita%2C+Norio%22">Narita, Norio</searchLink><br /><searchLink fieldCode="AR" term="%22Palle%2C+Enric%22">Palle, Enric</searchLink><br /><searchLink fieldCode="AR" term="%22Kawai%2C+Yugo%22">Kawai, Yugo</searchLink><br /><searchLink fieldCode="AR" term="%22Baker%2C+D%2E%22">Baker, D.</searchLink>
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  Data: <i>Exoplaneter från rymden - CHEOPS och PLATO, ESA's nästa två rymdteleskop (fas 2) Astronomy and Astrophysics Additional tables: Obliquities of exoplanet host stars. Nineteen new, updated measurements for the sample of 205 measurements and observed trends</i>. 690
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  Data: <searchLink fieldCode="DE" term="%22Planet-star+interactions%22">Planet-star interactions</searchLink><br /><searchLink fieldCode="DE" term="%22Planets+and+satellites%3A+dynamical+evolution+and+stability%22">Planets and satellites: dynamical evolution and stability</searchLink><br /><searchLink fieldCode="DE" term="%22Planets+and+satellites%3A+formation%22">Planets and satellites: formation</searchLink>
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  Data: Measurements of the obliquities in exoplanet systems have revealed some remarkable architectures, some of which are very different from the Solar System. Nearly 200 obliquity measurements have been obtained through observations of the Rossiter McLaughlin (RM) effect. Here, we report on observations of 19 planetary systems that led to 17 clear detections of the RM effect and 2 less secure detections. After adding the new measurements to the tally, we used the entire collection of RM measurements to investigate four issues that have arisen in the literature. i) Does the obliquity distribution show a peak at approximately 90 ? We find tentative evidence that such a peak does exist when restricting attention to the sample of sub-Saturn planets and hot Jupiters orbiting F stars. ii) Are high obliquities associated with high eccentricities? We find the association to be weaker than previously reported, and that a stronger association exists between obliquity and orbital separation, possibly due to tidal obliquity damping at small separations. iii) How low are the lowest known obliquities? Among hot Jupiters around cool stars, we find the dispersion to be 1.4 ± 0.7, smaller than the 6 obliquity of the Sun, which serves as additional evidence for tidal damping. iv) What are the obliquities of stars with compact and flat systems of multiple planets? We find that they generally have obliquities lower than 10, with several remarkable exceptions possibly caused by wide-orbiting stellar or planetary companions.
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