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Dive into the research topics where Emeline Bolmont is active.

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Featured researches published by Emeline Bolmont.


Nature | 2017

Seven temperate terrestrial planets around the nearby ultracool dwarf star TRAPPIST-1

Michaël Gillon; A. H. M. J. Triaud; Brice-Olivier Demory; Emmanuel Jehin; Eric Agol; Katherine M. Deck; Susan M. Lederer; Julien de Wit; Artem Burdanov; James G. Ingalls; Emeline Bolmont; Jérémy Leconte; Sean N. Raymond; Franck Selsis; Martin Turbet; Khalid Barkaoui; Adam J. Burgasser; M. R. Burleigh; Sean J. Carey; Aleksander Chaushev; C. M. Copperwheat; Laetitia Delrez; Catarina S. Fernandes; Daniel L. Holdsworth; Enrico J. Kotze; Valérie Van Grootel; Yaseen Almleaky; Z. Benkhaldoun; Pierre Magain; D. Queloz

One aim of modern astronomy is to detect temperate, Earth-like exoplanets that are well suited for atmospheric characterization. Recently, three Earth-sized planets were detected that transit (that is, pass in front of) a star with a mass just eight per cent that of the Sun, located 12 parsecs away. The transiting configuration of these planets, combined with the Jupiter-like size of their host star—named TRAPPIST-1—makes possible in-depth studies of their atmospheric properties with present-day and future astronomical facilities. Here we report the results of a photometric monitoring campaign of that star from the ground and space. Our observations reveal that at least seven planets with sizes and masses similar to those of Earth revolve around TRAPPIST-1. The six inner planets form a near-resonant chain, such that their orbital periods (1.51, 2.42, 4.04, 6.06, 9.1 and 12.35 days) are near-ratios of small integers. This architecture suggests that the planets formed farther from the star and migrated inwards. Moreover, the seven planets have equilibrium temperatures low enough to make possible the presence of liquid water on their surfaces.


Science | 2014

An earth-sized planet in the habitable zone of a cool star

Elisa V. Quintana; Sean N. Raymond; Jason F. Rowe; Emeline Bolmont; Douglas A. Caldwell; Steve B. Howell; Stephen R. Kane; Daniel Huber; Justin R. Crepp; Jack J. Lissauer; David R. Ciardi; Jeffrey L. Coughlin; Mark E. Everett; Christopher E. Henze; Elliott P. Horch; Howard Isaacson; Eric B. Ford; Fred C. Adams; Martin Still; Roger C. Hunter; Billy Quarles; Franck Selsis

Starry Brightness The high photometric precision of NASAs Kepler observatory has enabled the detection of many planets because they cause slight dimming of their host stars as they orbit in front of them. From these data, Quintana et al. (p. 277) have spotted a five-planet system around a small star. Here, the outermost planet is only 10% larger than Earth and completes its 130-day orbit entirely within the habitable zone, where liquid water could exist on its surface. Similarly, Kepler can detect faint periodic brightenings, as Kruse and Agol (p. 275) have reported for the binary system KOI-3278. In this system, a white dwarf acts as a gravitational microlens when it passes in front of its Sun-like G-star companion every 88 days. The lensing effect allows the mass of the white dwarf to be estimated, which helps us to understand how similar binary systems may have evolved. NASA’s Kepler mission revealed that the fifth and outermost planet orbiting Kepler-186 is capable of hosting liquid water. The quest for Earth-like planets is a major focus of current exoplanet research. Although planets that are Earth-sized and smaller have been detected, these planets reside in orbits that are too close to their host star to allow liquid water on their surfaces. We present the detection of Kepler-186f, a 1.11 ± 0.14 Earth-radius planet that is the outermost of five planets, all roughly Earth-sized, that transit a 0.47 ± 0.05 solar-radius star. The intensity and spectrum of the star’s radiation place Kepler-186f in the stellar habitable zone, implying that if Kepler-186f has an Earth-like atmosphere and water at its surface, then some of this water is likely to be in liquid form.


Astronomy and Astrophysics | 2016

The habitability of Proxima Centauri b. I. Irradiation, rotation and volatile inventory from formation to the present

Ignasi Ribas; Emeline Bolmont; Franck Selsis; Ansgar Reiners; Jérémy Leconte; Sean N. Raymond; Scott G. Engle; Edward F. Guinan; J. Morin; Martin Turbet; F. Forget; Guillem Anglada-Escudé

Proxima b is a planet with a minimum mass of 1.3 MEarth orbiting within the habitable zone (HZ) of Proxima Centauri, a very low-mass, active star and the Suns closest neighbor. Here we investigate a number of factors related to the potential habitability of Proxima b and its ability to maintain liquid water on its surface. We set the stage by estimating the current high-energy irradiance of the planet and show that the planet currently receives 30 times more EUV radiation than Earth and 250 times more X-rays. We compute the time evolution of the stars spectrum, which is essential for modeling the flux received over Proxima bs lifetime. We also show that Proxima bs obliquity is likely null and its spin is either synchronous or in a 3:2 spin-orbit resonance, depending on the planets eccentricity and level of triaxiality. Next we consider the evolution of Proxima bs water inventory. We use our spectral energy distribution to compute the hydrogen loss from the planet with an improved energy-limited escape formalism. Despite the high level of stellar activity we find that Proxima b is likely to have lost less than an Earth oceans worth of hydrogen before it reached the HZ 100-200 Myr after its formation. The largest uncertainty in our work is the initial water budget, which is not constrained by planet formation models. We conclude that Proxima b is a viable candidate habitable planet.


Astronomy and Astrophysics | 2016

The habitability of Proxima Centauri b. II. Possible climates and Observability

Martin Turbet; Jérémy Leconte; Franck Selsis; Emeline Bolmont; F. Forget; Ignasi Ribas; Sean N. Raymond; Guillem Anglada-Escudé

Radial velocity monitoring has found the signature of a


Astrobiology | 2014

Formation, Habitability, and Detection of Extrasolar Moons

René Heller; Darren M. Williams; David M. Kipping; Mary Anne Limbach; Edwin L. Turner; Richard Greenberg; T. Sasaki; Emeline Bolmont; Olivier Grasset; Karen M. Lewis; Rory Barnes; Jorge I. Zuluaga

M \sin i = 1.3


Nature Astronomy | 2017

A seven-planet resonant chain in TRAPPIST-1

Rodrigo Luger; Marko Sestovic; Ethan Kruse; Simon L. Grimm; Brice-Olivier Demory; Eric Agol; Emeline Bolmont; Daniel C. Fabrycky; Catarina S. Fernandes; Valérie Van Grootel; Adam J. Burgasser; Michaël Gillon; James G. Ingalls; Emmanuel Jehin; Sean N. Raymond; Franck Selsis; A. H. M. J. Triaud; Geert Barentsen; Steve B. Howell; Laetitia Delrez; Julien de Wit; Daniel Foreman-Mackey; Daniel L. Holdsworth; Jérémy Leconte; Susan M. Lederer; Martin Turbet; Yaseen Almleaky; Z. Benkhaldoun; Pierre Magain; Brett M. Morris

~M


Nature | 2016

A map of the large day–night temperature gradient of a super-Earth exoplanet

Brice-Olivier Demory; Michaël Gillon; Julien de Wit; Nikku Madhusudhan; Emeline Bolmont; Kevin Heng; Tiffany Kataria; Nikole K. Lewis; Renyu Hu; Jessica E. Krick; Vlada Stamenković; Björn Benneke; Stephen R. Kane; D. Queloz

_\oplus


Monthly Notices of the Royal Astronomical Society | 2017

Water loss from terrestrial planets orbiting ultracool dwarfs: implications for the planets of TRAPPIST-1

Emeline Bolmont; Franck Selsis; James E. Owen; Ignasi Ribas; Sean N. Raymond; Jérémy Leconte; Michaël Gillon

planet located within the Habitable Zone (HZ) of Proxima Centauri \citep{Anglada16}. Despite a hotter past and an active host star the planet Proxima~b could have retained enough volatiles to sustain surface habitability \citep{Ribas2016}. Here we use a 3D Global Climate Model (GCM) to simulate Proxima bs atmosphere and water cycle for its two likely rotation modes (1:1 and 3:2 spin-orbit resonances) while varying the unconstrained surface water inventory and atmospheric greenhouse effect. We find that a broad range of atmospheric compositions allow surface liquid water. On a tidally-locked planet with sufficient surface water inventory, liquid water is always present, at least in the substellar region. With a non-synchronous rotation, this requires a minimum greenhouse warming (


Astronomy and Astrophysics | 2012

Effect of the stellar spin history on the tidal evolution of close-in planets

Emeline Bolmont; Sean N. Raymond; Jérémy Leconte; Sean P. Matt

\sim


Astronomy and Astrophysics | 2017

Reconnaissance of the TRAPPIST-1 exoplanet system in the Lyman-α line

V. Bourrier; D. Ehrenreich; P. J. Wheatley; Emeline Bolmont; Michaël Gillon; J. de Wit; Adam J. Burgasser; Emmanuel Jehin; D. Queloz; A. H. M. J. Triaud

10~mbar of CO

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Jérémy Leconte

Centre national de la recherche scientifique

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Franck Selsis

Centre national de la recherche scientifique

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Julien de Wit

Massachusetts Institute of Technology

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