scholarly journals Six transiting planets and a chain of Laplace resonances in TOI-178

2021 ◽  
Author(s):  
Adrien Leleu
Keyword(s):  
Planet Formation ◽  
Planetary Systems ◽  
Single System ◽  
Transiting Planets ◽  
Orbital Configuration ◽  
Resonant Systems ◽  
Formation And Evolution ◽  
A Chain ◽  
Formation Phase

<p class="p1">Determining the architecture of multi-planetary systems is one of the cornerstones of understanding planet formation and evolution. Resonant systems are especially important as the fragility of their orbital configuration ensures that no significant scattering or collisional event has taken place since the earliest formation phase when the parent protoplanetary disc was still present. As unveiled by TESS, CHEOPS, ESPRESSO, NGTS and SPECULOOS, TOI-178 harbours at least six planets in the super-Earth to mini-Neptune regimes, all planets but the innermost one form a 2:4:6:9:12 chain of Laplace resonances, and the planetary densities show important variations from planet to planet. TOI-178 have hence several characteristics that were not previously observed in a single system, making it a key system for the study of processes of formation and evolution of planetary systems. We will review what we know of TOI-178, and what we expect from futur observations.</p>

scholarly journals Detecting Extrasolar Planet Transits from the South Pole

2004 ◽  
Vol 213 ◽  
pp. 93-96
Author(s):  
Douglas A. Caldwell ◽  
William J. Borucki ◽  
Robert L. Showen ◽  
Jon M. Jenkins ◽  
Laurance Doyle ◽  
...  
Keyword(s):  
Radial Velocity ◽  
Planet Formation ◽  
Extrasolar Planet ◽  
Doppler Velocity ◽  
Wide Field ◽  
South Pole ◽  
The South ◽  
Transiting Planets ◽  
Formation And Evolution

We have developed and tested a wide-field photometer to detect extrasolar planet transits from the South Pole. The discovery of transiting planets for which masses can be measured by radial velocity is vital to constrain the models of planet formation and evolution. Short of going to space, the South Pole is the best site from which to carry out a such a survey. Based on results from the Doppler velocity surveys and the Vulcan transit search, we expect to detect 10 to 15 transiting planets in two years of operation at the South Pole.

scholarly journals The Complete Census of 70 μm–Bright Debris Disks within “The Formation and Evolution of Planetary Systems”SpitzerLegacy Survey of Sun‐like Stars

2008 ◽  
Vol 677 (1) ◽  
pp. 630-656 ◽  
Author(s):  
Lynne A. Hillenbrand ◽  
John M. Carpenter ◽  
Jinyoung Serena Kim ◽  
Michael R. Meyer ◽  
Dana E. Backman ◽  
...  
Keyword(s):  
Planetary Systems ◽  
Debris Disks ◽  
Formation And Evolution

How many suns are in the sky? Multiplicity surveys of exoplanet host stars

2018 ◽  
Vol 14 (S345) ◽  
pp. 316-317 ◽  
Author(s):  
M. Mugrauer ◽  
C. Ginski ◽  
N. Vogt ◽  
R. Neuhäuser ◽  
C. Adam
Keyword(s):  
Milky Way ◽  
Planet Formation ◽  
High Contrast ◽  
Contrast Imaging ◽  
Direct Imaging ◽  
High Contrast Imaging ◽  
Multiple Stars ◽  
First Results ◽  
Formation And Evolution ◽  
Host Stars

AbstractIn order to determine the true impact of stellar multiplicity on the formation and evolution of planets, we initiated direct imaging surveys to search for (sub)stellar companions of exoplanet host stars on close orbits, as their gravitational impact on the planet bearing disk at first and on formed planets afterwards is expected to be maximal. According to theory these are the most challenging environments for planet formation and evolution but might occur quite frequently in the milky way, due to the large number of multiple stars within our galaxy. On this poster we showed results, obtained so far in the course of our AO and Lucky-imaging campaigns of exoplanet host stars, conducted with NACO/ESO-VLT for southern and with AstraLux/CAHA2.2m for northern targets, respectively. In addition, we introduced our new high contrast imaging survey with SPHERE/ESO-VLT to search for close companions of southern exoplanet host stars, and presented some first results.

Ages for large samples of stars - caveats and uncertainties

2017 ◽  
Vol 13 (S334) ◽  
pp. 147-152
Author(s):  
Arlette Noels-Grötsch
Keyword(s):  
Main Sequence ◽  
Planetary Systems ◽  
Foreseeable Future ◽  
Time Line ◽  
Giant Stars ◽  
Large Samples ◽  
Formation And Evolution ◽  
Stellar Models ◽  
Red Giant ◽  
Age Determinations

AbstractAlthough a stellar age accuracy of about 10 % seems to be a reasonable requirement to draw a time line in the evolution of our Galaxy as well as in the formation and evolution of exo-planetary systems, theoretical stellar models are at present still too imperfect to really achieve this goal. Asteroseismic observations are definitely of invaluable assistance, especially if individual pulsation frequencies are available, which is still far from common. Large stellar samples are now in the spotlight with two different lines of attack, spectroscopic and photometric surveys as well as asteroseismic missions. I shall review the problems arising from stellar physics in the context of large stellar samples of main sequence and red giant stars, and I shall raise some alarm bells but also highlight some positive news for a drastic improvement in stellar age determinations below the limit of 10 % in a foreseeable future.

scholarly journals Characterisation of exoplanet host stars: A window into planet formation

2017 ◽  
Vol 12 (S330) ◽  
pp. 369-376 ◽  
Author(s):  
Nuno C. Santos
Keyword(s):  
Planet Formation ◽  
The Sun ◽  
The Future ◽  
The Galaxy ◽  
Crucial Information ◽  
Formation And Evolution ◽  
Host Stars

AbstractThe detection of thousands of planets orbiting stars other than the Sun has shown that planets are common throughout the Galaxy. However, the diversity of systems found has also raised many questions regarding the process of planet formation and evolution. Interestingly, but perhaps not unexpectedly, crucial information to constraint the planet formation models comes from the analysis of the planet-host stars. In this talk I will review why it is so important to study and understand the stars when finding and characterising exoplanets. I will then present some of the most relevant star-planet relations found to date, and how they are helping us to understand planet formation and evolution. I will end with a presentation of the future steps in this field, including what Gaia will bring to help constrain the properties of planet-host stars, as well as to the star-planet connection.

scholarly journals Revisited mass-radius relations for exoplanets below 120 M⊕

2020 ◽  
Vol 634 ◽  
pp. A43 ◽  
Author(s):  
J. F. Otegi ◽  
F. Bouchy ◽  
R. Helled
Keyword(s):  
Pure Water ◽  
Mass Range ◽  
Planetary Formation ◽  
Core Mass ◽  
Transiting Planets ◽  
Small Density ◽  
Different Populations ◽  
Formation And Evolution ◽  
The Masses ◽  
Two Populations

The masses and radii of exoplanets are fundamental quantities needed for their characterisation. Studying the different populations of exoplanets is important for understanding the demographics of the different planetary types, which can then be linked to planetary formation and evolution. We present an updated exoplanet catalogue based on reliable, robust, and, as much as possible accurate mass and radius measurements of transiting planets up to 120 M⊕. The resulting mass-radius (M-R) diagram shows two distinct populations, corresponding to rocky and volatile-rich exoplanets which overlap in both mass and radius. The rocky exoplanet population shows a relatively small density variability and ends at mass of ~25 M⊕, possibly indicating the maximum core mass that can be formed. We use the composition line of pure water to separate the two populations, and infer two new empirical M-R relations based on this data: M = (0.9 ± 0.06) R(3.45±0.12) for the rocky population, and M = (1.74 ± 0.38) R(1.58±0.10) for the volatile-rich population. While our results for the two regimes are in agreement with previous studies, the new M-R relations better match the population in the transition region from rocky to volatile-rich exoplanets, which correspond to a mass range of 5–25 M⊕, and a radius range of 2–3 R⊕.

scholarly journals Habitable Planet Formation in Binary Planetary Systems

2007 ◽  
Vol 666 (1) ◽  
pp. 436-446 ◽  
Author(s):  
Nader Haghighipour ◽  
Sean N. Raymond
Keyword(s):  
Planet Formation ◽  
Planetary Systems ◽  
Habitable Planet

scholarly journals N-body Simulations of Planet Formation

2003 ◽  
Vol 208 ◽  
pp. 25-35 ◽  
Author(s):  
Shigeru Ida ◽  
Eiichiro Kokubo ◽  
Junko Kominami
Keyword(s):  
Final Stage ◽  
Planet Formation ◽  
Planetary Systems ◽  
Terrestrial Planet ◽  
The Other ◽  
Other Hand ◽  
Giant Impacts ◽  
Gas Accretion

Accretion from many small planetesimals to planets is reviewed. Solid protoplanets accrete through runaway and oligarchic growth until they become isolated. The isolation mass of protoplanets in terrestrial planet region is about 0.1-0.2 Earth mass, which suggests giant impacts among the protoplanets in the final stage of terrestrial planet formation. On the other hand, the isolation mass in Jupiter's and Saturn's orbits is about a few to 5 Earth masses, which may be massive enough to trigger gas accretion onto the cores. The isolation mass in Uranus and Neptune's orbits is as large as their present cores. Extending the above arguments to extrasolar planetary systems that are formed from disks with various initial masses, we also discuss diversity of extrasolar planetary systems.

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