Accretion of planetary matter from debris disks around white dwarfs: the fate of planetary systems

2013 ◽  
Vol 63 ◽  
pp. 297-302
Author(s):  
M. Deal ◽  
S. Deheuvels ◽  
G. Vauclair ◽  
S. Vauclair ◽  
F.C. Wachlin
Keyword(s):  
White Dwarfs ◽  
Planetary Systems ◽  
Debris Disks

scholarly journals Bayesian constraints on the origin and geology of exo-planetary material using a population of externally polluted white dwarfs

2021 ◽  
Author(s):  
John H D Harrison ◽  
Amy Bonsor ◽  
Mihkel Kama ◽  
Andrew M Buchan ◽  
Simon Blouin ◽  
...  
Keyword(s):  
Solar System ◽  
White Dwarf ◽  
Bayesian Model ◽  
Total Mass ◽  
White Dwarfs ◽  
Bulk Composition ◽  
Planetary Systems ◽  
The Moon ◽  
Planetary Bodies ◽  
Nearby Stars

Abstract White dwarfs that have accreted planetary bodies are a powerful probe of the bulk composition of exoplanetary material. In this paper, we present a Bayesian model to explain the abundances observed in the atmospheres of 202 DZ white dwarfs by considering the heating, geochemical differentiation, and collisional processes experienced by the planetary bodies accreted, as well as gravitational sinking. The majority (>60%) of systems are consistent with the accretion of primitive material. We attribute the small spread in refractory abundances observed to a similar spread in the initial planet-forming material, as seen in the compositions of nearby stars. A range in Na abundances in the pollutant material is attributed to a range in formation temperatures from below 1,000 K to higher than 1,400 K, suggesting that pollutant material arrives in white dwarf atmospheres from a variety of radial locations. We also find that Solar System-like differentiation is common place in exo-planetary systems. Extreme siderophile (Fe, Ni or Cr) abundances in 8 systems require the accretion of a core-rich fragment of a larger differentiated body to at least a 3σ significance, whilst one system shows evidence that it accreted a crust-rich fragment. In systems where the abundances suggest that accretion has finished (13/202), the total mass accreted can be calculated. The 13 systems are estimated to have accreted masses ranging from the mass of the Moon to half that of Vesta. Our analysis suggests that accretion continues for 11Myrs on average.

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

scholarly journals Planet forming disks, debris disks and the Solar System

2019 ◽  
Vol 15 (S350) ◽  
pp. 207-215
Author(s):  
Inga Kamp
Keyword(s):  
Chemical Composition ◽  
Solar System ◽  
Planetary Systems ◽  
Theoretical Work ◽  
Structure Evolution ◽  
Debris Disks ◽  
Physical Processes ◽  
Disk Structure ◽  
Open Questions ◽  
Evolution Modeling

AbstractVLT instruments and ALMA with their high spatial resolution have revolutionized in the past five years our view and understanding of how disks turn into planetary systems. This talk will briefly outline our current understanding of the physical processes occurring and chemical composition evolving as these disks turn into debris disks and eventually planetary systems like our own solar system. I will especially focus on the synergy between disk structure/evolution modeling and astrochemical laboratory/theoretical work to highlight the most recent advances, and open questions such as (1) how much of the chemical composition in disks is inherited from molecular clouds, (2) the relevance of snowlines for planet formation, and (3) what is the origin of the gas in debris disks and what can we learn from it. For each of the three, I will outline briefly how the combination of theory/lab astrochemistry, astrophysical models and observations are required to advance our understanding.

scholarly journals White dwarfs with unresolved substellar companions and debris disks in the UKIDSS Survey

2009 ◽  
Vol 172 ◽  
pp. 012058 ◽  
Author(s):  
Paul Steele ◽  
Matt Burleigh ◽  
Martin Barstow ◽  
Richard Jameson ◽  
Paul Dobbie
Keyword(s):  
White Dwarfs ◽  
Debris Disks ◽  
Substellar Companions

Analysis of the Chemical Composition of the Atmospheres of Stars with Debris Disks and Planetary Systems

Astrophysics ◽  
2013 ◽  
Vol 56 (4) ◽  
pp. 461-471
Author(s):  
M. Rojas ◽  
N. A. Drake ◽  
C. Chavero ◽  
C. B. Pereira ◽  
A. F. Kholtygin ◽  
...  
Keyword(s):  
Chemical Composition ◽  
Planetary Systems ◽  
Debris Disks

scholarly journals THE FREQUENCY OF DEBRIS DISKS AT WHITE DWARFS

2012 ◽  
Vol 760 (1) ◽  
pp. 26 ◽  
Author(s):  
Sara D. Barber ◽  
Adam J. Patterson ◽  
Mukremin Kilic ◽  
S. K. Leggett ◽  
P. Dufour ◽  
...  
Keyword(s):  
White Dwarfs ◽  
Debris Disks

scholarly journals Characterizing planetesimal belts through the study of debris dust

2010 ◽  
Vol 6 (S276) ◽  
pp. 54-59
Author(s):  
Amaya Moro-Martín
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Planetary Systems ◽  
Dust Particles ◽  
Debris Disks ◽  
Main Sequence Stars ◽  
Wide Range ◽  
Robust Process

AbstractMain sequence stars are commonly surrounded by disks of dust. From lifetime arguments, it is inferred that the dust particles are not primordial but originate from the collision of planetesimals, similar to the asteroids, comets and KBOs in our Solar system. The presence of these debris disks around stars with a wide range of masses, luminosities, and metallicities, with and without binary companions, is evidence that planetesimal formation is a robust process that can take place under a wide range of conditions. Debris disks can help us learn about the formation, evolution and diversity of planetary systems.

scholarly journals Non-LTE Model Spectra for Gaseous Planetary Debris Disks around WDs

2013 ◽  
Vol 8 (S299) ◽  
pp. 342-343
Author(s):  
Stephan Hartmann ◽  
Thorsten Nagel ◽  
Thomas Rauch ◽  
Klaus Werner
Keyword(s):  
Accretion Disk ◽  
Effective Temperature ◽  
Surface Density ◽  
White Dwarfs ◽  
Debris Disks ◽  
Chemical Mixture ◽  
Dust Disks ◽  
Infrared Triplet ◽  
Do So

AbstractMetal-rich dust disks around white dwarfs are thought to be the debris of tidally disrupted rocky bodies. While normally the number of features to study the planetary material directly is very limited, ancillary gas disks around some of these white dwarfs provide the opportunity to do so. We used our Tübingen Accretion Disk code AcDc, assuming non-LTE conditions, to model the gaseous spectrum component. We investigated the chemical mixture as well as the surface density and effective temperature, and utilized the Ca ii infrared triplet to determine the geometry of the disk.

scholarly journals PROBING THE TERRESTRIAL REGIONS OF PLANETARY SYSTEMS: WARM DEBRIS DISKS WITH EMISSION FEATURES

2014 ◽  
Vol 793 (1) ◽  
pp. 57 ◽  
Author(s):  
Nicholas P. Ballering ◽  
George H. Rieke ◽  
András Gáspár
Keyword(s):  
Planetary Systems ◽  
Debris Disks
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