Transits Probabilities Around Hypervelocity and Runaway Stars

Abstract

In the blooming field of exoplanetary science, NASA's Kepler Space Telescope has revolutionized our understanding of exoplanets. Kepler's very precise and long-duration photometry is ideal for detecting planetary transits around Sun-like stars. The forthcoming Transiting Exoplanet Survey Satellite (TESS) is expected to continue Kepler's legacy. Along with transits, the Doppler technique remains an invaluable tool for discovering planets. The next generation of spectrographs, such as G-CLEF, promises precision radial velocity measurements. In this paper, we explore the possibility of detecting planets around hypervelocity and runaway stars, which should host a very compact system as consequence of their turbulent origin. We find that the probability of a multi-planetary transit is $10^{-3}\lesssim P\lesssim 10^{-1}$. We therefore need to observe $\sim 10-1000$ high-velocity stars to spot a transit. However, even if transits are rare around runaway and hypervelocity stars, the chances of detecting such planets using radial velocity surveys is high. We predict that the European Gaia satellite, along with TESS and the new-generation spectrographs G-CLEF and ESPRESSO, will spot planetary systems orbiting high-velocity stars.

arXiv comment10 pages, 6 figures, accepted for publication in MNRAS

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Cited by in corpus (10)

• Gravitational Waves and Intermediate-mass Black Hole Retention in Globular Clusters
• Galactic Panspermia
• Constraining Milky Way mass with Hypervelocity Stars
• Hypervelocity stars from young stellar clusters in the Galactic Centre
• Steeper stellar cusps in galactic centers from binary disruption
• The secular tidal disruption of stars by low-mass Super Massive Black Holes secondaries in galactic nuclei
• Tidal breakup of triple stars in the Galactic Centre
• Tidal breakup of quadruple stars in the Galactic Centre
• A Candidate High-Velocity Exoplanet System in the Galactic Bulge
• The Fate of Binary Stars Hosting Planets upon Interaction with Sgr A* Black hole