β Pictoris and other star spectra, in connection with planet formation

2004 ◽  
Vol 202 ◽  
pp. 300-307
Author(s):  
Anne. M. Lagrange ◽  
Herve Beust
Keyword(s):  
Planet Formation ◽  
Planetary System ◽  
Present Knowledge ◽  
Debris Disks ◽  
System Activity ◽  
Pms Stars

We review here the present knowledge on the gaseous phases of debris disks found around MS and old PMS stars, and make an attempt to connect them with planetary system activity.

scholarly journals Abundances in Stars with Debris Disks

2013 ◽  
Vol 8 (S299) ◽  
pp. 356-357
Author(s):  
Adam M. Ritchey ◽  
Guillermo Gonzalez ◽  
Myra Stone ◽  
George Wallerstein
Keyword(s):  
Planet Formation ◽  
Giant Planet ◽  
Infrared Emission ◽  
Stellar Atmospheres ◽  
Elemental Abundance ◽  
Condensation Temperature ◽  
Debris Disks ◽  
Chemical Abundance ◽  
Preliminary Results ◽  
Solar Type

AbstractWe present preliminary results of a detailed chemical abundance analysis for a sample of solar-type stars known to exhibit excess infrared emission associated with dusty debris disks. Our sample of 28 stars was selected based on results from the Formation and Evolution of Planetary Systems (FEPS) Spitzer Legacy Program, for the purpose of investigating whether the stellar atmospheres have been polluted with planetary material, which could indicate that the metallicity enhancement in stars with planets is due to metal-rich infall in the later stages of star and planet formation. The preliminary results presented here consist of precise abundances for 15 elements (C, O, Na, Mg, Al, Si, S, Ca, Sc, Ti, V, Cr, Fe, Co, and Ni) for half of the stars in our sample. We find that none of the stars investigated so far exhibit the expected trend of increasing elemental abundance with increasing condensation temperature, which would result from the stars having accreted planetary debris. Rather, the slopes of linear least-squares fits to the abundance data are either negative or consistent with zero. In both cases, our results may indicate that, like the Sun, the debris disk host stars are deficient in refractory elements, a possible signature of terrestrial and/or gas giant planet formation.

scholarly journals Debris disks as signposts of terrestrial planet formation

2012 ◽  
Vol 541 ◽  
pp. A11 ◽  
Author(s):  
S. N. Raymond ◽  
P. J. Armitage ◽  
A. Moro-Martín ◽  
M. Booth ◽  
M. C. Wyatt ◽  
...  
Keyword(s):  
Planet Formation ◽  
Terrestrial Planet ◽  
Debris Disks

scholarly journals The TROY project

2018 ◽  
Vol 618 ◽  
pp. A42 ◽  
Author(s):  
J. Lillo-Box ◽  
A. Leleu ◽  
H. Parviainen ◽  
P. Figueira ◽  
M. Mallonn ◽  
...  
Keyword(s):  
Solar System ◽  
Radial Velocity ◽  
Parameter Space ◽  
Planet Formation ◽  
Planetary System ◽  
Lagrangian Points ◽  
Formation And Evolution ◽  
Observing Techniques

Context.Co-orbital bodies are the byproduct of planet formation and evolution, as we know from the solar system. Although planet-size co-orbitals do not exists in our planetary system, dynamical studies show that they can remain stable for long periods of time in the gravitational well of massive planets. Should they exist, their detection is feasible with the current instrumentation.Aims.In this paper, we present new ground-based observations searching for these bodies co-orbiting with nine close-in (P< 5 days) planets, using various observing techniques. The combination of all of these techniques allows us to restrict the parameter space of any possible trojan in the system.Methods.We used multi-technique observations, comprised of radial velocity, precision photometry, and transit timing variations, both newly acquired in the context of the TROY project and publicly available, to constrain the presence of planet-size trojans in the Lagrangian points of nine known exoplanets.Results.We find no clear evidence of trojans in these nine systems through any of the techniques used down to the precision of the observations. However, this allows us to constrain the presence of any potential trojan in the system, especially in the trojan mass or radius vs. libration amplitude plane. In particular, we can set upper mass limits in the super-Earth mass regime for six of the studied systems.

scholarly journals Planetary Systems Dynamics Eccentric patterns in debris disks & Planetary migration in binary systems

2013 ◽  
Vol 8 (S299) ◽  
pp. 212-213
Author(s):  
V. Faramaz ◽  
H. Beust ◽  
J.-C. Augereau ◽  
A. Bonsor ◽  
P. Thébault ◽  
...  
Keyword(s):  
Binary Systems ◽  
Planet Formation ◽  
Planetary Systems ◽  
Systems Dynamics ◽  
Debris Disks ◽  
Space Observatory ◽  
Herschel Space Observatory ◽  
Migration Mechanism ◽  
Planetary Migration

AbstractWe present some highlights of two ongoing investigations that deal with the dynamics of planetary systems. Firstly, until recently, observed eccentric patterns in debris disks were found in young systems. However recent observations of Gyr-old eccentric debris disks leads to question the survival timescale of this type of asymmetry. One such disk was recently observed in the far-IR by the Herschel Space Observatory around ζ2 Reticuli. Secondly, as a binary companion orbits a circumprimary disk, it creates regions where planet formation is strongly handicapped. However, some planets were detected in this zone in tight binary systems (γ Cep, HD 196885). We aim to determine whether a binary companion can affect migration such that planets are brought in these regions and focus in particular on the planetesimal-driven migration mechanism.

scholarly journals Insights into Planet Formation from Debris Disks

2016 ◽  
Vol 205 (1-4) ◽  
pp. 231-265 ◽  
Author(s):  
Mark C. Wyatt ◽  
Alan P. Jackson
Keyword(s):  
Planet Formation ◽  
Debris Disks

scholarly journals Radio Interferometry Observations of the Hallmarks of Planet Formation

2013 ◽  
Vol 8 (S299) ◽  
pp. 80-89
Author(s):  
Sean M. Andrews
Keyword(s):  
Planet Formation ◽  
Angular Resolution ◽  
Planetary System ◽  
Planetary Systems ◽  
Protoplanetary Disks ◽  
Circumstellar Disks ◽  
High Angular Resolution ◽  
Radio Interferometry ◽  
New Directions ◽  
And Migration

AbstractSome of the fundamental processes involved in the evolution of circumstellar disks and the assembly of planetary systems are just now becoming accessible to astronomical observations. The new promise of observational work in the field of planet formation makes for a very dynamic research scenario, which is certain to be amplified in the coming years as the revolutionary Atacama Large Millimeter/submillimeter Array (ALMA) facility ramps up to full operations. To highlight the new directions being explored in these fields, this brief review will describe how high angular resolution measurements at millimeter/radio wavelengths are being used to study several crucial aspects of the formation and early evolution of planetary systems, including: the gas and dust structures of protoplanetary disks, the growth and migration of disk solids, and the interactions between a young planetary system and its natal, gas-rich disk.

scholarly journals The tidal parameters of TRAPPIST-1b and c

2019 ◽  
Vol 487 (1) ◽  
pp. 34-47 ◽  
Author(s):  
R Brasser ◽  
A C Barr ◽  
V Dobos
Keyword(s):  
Planet Formation ◽  
Planetary System ◽  
Tidal Evolution ◽  
Secular Theory ◽  
Planet Migration ◽  
Dynamical Simulations ◽  
Synchronous Rotation ◽  
History Of ◽  
The Masses

Abstract The TRAPPIST-1 planetary system consists of seven planets within 0.05 au of each other, five of which are in a multiresonant chain. These resonances suggest the system formed via planet migration; subsequent tidal evolution has damped away most of the initial eccentricities. We used dynamical N-body simulations to estimate how long it takes for the multiresonant configuration that arises during planet formation to break. From there we use secular theory to pose limits on the tidal parameters of planets b and c. We calibrate our results against multilayered interior models constructed to fit the masses and radii of the planets, from which the tidal parameters are computed independently. The dynamical simulations show that the planets typically go unstable 30 Myr after their formation. Assuming synchronous rotation throughout, we compute $\frac{k_2}{Q} \gtrsim 2\times 10^{-4}$ for planet b and $\frac{k_2}{Q} \gtrsim 10^{-3}$ for planet c. Interior models yield (0.075–0.37) × 10−4 for TRAPPIST-1b and (0.4–2) × 10−4 for TRAPPIST-1c. The agreement between the dynamical and interior models is not too strong, but is still useful to constrain the dynamical history of the system. We suggest that this two-pronged approach could be of further use in other multiresonant systems if the planet’s orbital and interior parameters are sufficiently well known.

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