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 Debris Disks: Structure, Composition, and Variability

2018 ◽  
Vol 56 (1) ◽  
pp. 541-591 ◽  
Author(s):  
A. Meredith Hughes ◽  
Gaspard Duchêne ◽  
Brenda C. Matthews
Keyword(s):  
Main Sequence ◽  
Scattered Light ◽  
Kuiper Belt ◽  
Debris Disks ◽  
Main Sequence Stars ◽  
Zodiacal Light ◽  
Wide Range ◽  
The Masses ◽  
Insight Into ◽  
Short Days

Debris disks are tenuous, dust-dominated disks commonly observed around stars over a wide range of ages. Those around main sequence stars are analogous to the Solar System's Kuiper Belt and zodiacal light. The dust in debris disks is believed to be continuously regenerated, originating primarily with collisions of planetesimals. Observations of debris disks provide insight into the evolution of planetary systems; and the composition of dust, comets, and planetesimals outside the Solar System; as well as placing constraints on the orbital architecture and potentially the masses of exoplanets that are not otherwise detectable. This review highlights recent advances in multiwavelength, high-resolution scattered light and thermal imaging that have revealed a complex and intricate diversity of structures in debris disks and discusses how modeling methods are evolving with the breadth and depth of the available observations. Two rapidly advancing subfields highlighted in this review include observations of atomic and molecular gas around main sequence stars and variations in emission from debris disks on very short (days to years) timescales, providing evidence of non-steady-state collisional evolution particularly in young debris disks.

scholarly journals Origins of Hot Jupiters

2018 ◽  
Vol 56 (1) ◽  
pp. 175-221 ◽  
Author(s):  
Rebekah I. Dawson ◽  
John Asher Johnson
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Planetary Systems ◽  
Main Sequence Stars ◽  
High Eccentricity ◽  
Hot Jupiters ◽  
In Situ Formation ◽  
Tidal Migration ◽  
Hot Jupiter

Hot Jupiters were the first exoplanets to be discovered around main sequence stars and astonished us with their close-in orbits. They are a prime example of how exoplanets have challenged our textbook, solar-system inspired story of how planetary systems form and evolve. More than twenty years after the discovery of the first hot Jupiter, there is no consensus on their predominant origin channel. Three classes of hot Jupiter creation hypotheses have been proposed: in situ formation, disk migration, and high-eccentricity tidal migration. Although no origin channel alone satisfactorily explains all the evidence, two major origin channels together plausibly account for properties of hot Jupiters themselves and their connections to other exoplanet populations.

scholarly journals Testing the Vainshtein mechanism using stars and galaxies

2015 ◽  
Vol 24 (12) ◽  
pp. 1544021 ◽  
Author(s):  
Jeremy Sakstein ◽  
Kazuya Koyama
Keyword(s):  
General Relativity ◽  
Solar System ◽  
Main Sequence ◽  
Alternative Theories Of Gravity ◽  
The Novel ◽  
Main Sequence Stars ◽  
Cosmic Expansion ◽  
Astrophysical Objects ◽  
Theories Of Gravity ◽  
Alternative Theories

The Vainshtein mechanism is of paramount importance in many alternative theories of gravity. It hides deviations from general relativity (GR) in the solar system while allowing them to drive the acceleration of the cosmic expansion. Recently, a class of theories have emerged where the mechanism is broken inside astrophysical objects. In this essay, we look for novel probes of these theories by deriving the modified properties of stars and galaxies. We show that main-sequence stars are colder, less luminous and more ephemeral than GR predicts. Furthermore, the circular velocities of objects orbiting inside galaxies are slower and the lensing of light is weaker. We discuss the prospects for testing these theories using the novel phenomena presented here in light of current astrophysical surveys.

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.

EXPANDING THE CHARA/FLUOR HOT DISKS SURVEY

2013 ◽  
Vol 02 (02) ◽  
pp. 1340010 ◽  
Author(s):  
B. MENNESSON ◽  
N. SCOTT ◽  
T. TEN BRUMMELAAR ◽  
G. BRYDEN ◽  
N. TURNER ◽  
...  
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Near Infrared ◽  
Dust Cloud ◽  
Main Sequence Stars ◽  
Second Development ◽  
Zodiacal Dust ◽  
Dust Component ◽  
Initial Survey ◽  
Better Than

Little is presently known about the hot (>300 K) dust component of debris disks surrounding main sequence stars, similar to the zodiacal dust cloud found in the inner solar system. While extensive surveys have been carried out from space, the majority of detections have surprisingly come from the ground, where near infrared interferometric observations have recently revealed small (~1%) resolved excesses around a dozen nearby main sequence stars. Most of these results have come from the CHARA array "FLUOR" instrument (Mt. Wilson, CA), which has demonstrated the best sensitivity worldwide so far for this type of studies, and has carried out an initial survey of ~40 stars. In order to further understand the origin of this "hot dust phenomenon", we will extend this initial survey to a larger number of stars and lower excess detection limits, i.e. higher visibility accuracy providing higher contrast measurements. To this end, two major instrumental developments are underway at CHARA. The first one aims at improving FLUOR's sensitivity to a median K-band magnitude limit of 5 (making 200 targets available). The second development is based on a method that we recently developed for accurate (better than 0.1%) null depth measurements of stars, and that can be extended to regular interferometric visibility measurements.

Disappearance of stellar debris disks around main-sequence stars after 400 million years

Nature ◽  
10.1038/46749 ◽  
1999 ◽  
Vol 401 (6752) ◽  
pp. 456-458 ◽  
Author(s):  
H. J. Habing ◽  
C. Dominik ◽  
M. Jourdain de Muizon ◽  
M. F. Kessler ◽  
R. J. Laureijs ◽  
...  
Keyword(s):  
Main Sequence ◽  
Debris Disks ◽  
Main Sequence Stars

scholarly journals Planetary Systems

1999 ◽  
Vol 172 ◽  
pp. 313-316
Author(s):  
Pawel Artymowicz
Keyword(s):  
Radial Velocity ◽  
Main Sequence ◽  
Direct Evidence ◽  
Planetary System ◽  
Planetary Systems ◽  
Main Sequence Stars ◽  
The Past ◽  
Exoplanetary Systems ◽  
Beta Pictoris

AbstractThe past decade brought direct evidence of the previously surmised exoplanetary systems. A variety of planetary system types exist those around pulsars, around both young and old main-sequence stars (as evidenced by planetesimal disks of the Beta Pictoris-type), and the mature giant exoplanets found in radial velocity surveys. The surprising diversity of the exoplanetary systems is addressed by several theories of their origin.

scholarly journals Searching for gas giant planets on Solar system scales – a NACO/APPL′-band survey of A- and F-type main-sequence stars

2015 ◽  
Vol 453 (3) ◽  
pp. 2534-2540 ◽  
Author(s):  
T. Meshkat ◽  
M. A. Kenworthy ◽  
M. Reggiani ◽  
S. P. Quanz ◽  
E. E. Mamajek ◽  
...  
Keyword(s):  
Solar System ◽  
Main Sequence ◽  
Giant Planets ◽  
Main Sequence Stars ◽  
Gas Giant ◽  
Band Survey

scholarly journals Candidate Main‐Sequence Stars with Debris Disks: A New Sample of Vega‐like Sources

1998 ◽  
Vol 497 (1) ◽  
pp. 330-341 ◽  
Author(s):  
Vincent Mannings ◽  
Michael J. Barlow
Keyword(s):  
Main Sequence ◽  
Debris Disks ◽  
Main Sequence Stars

Examples of Comet-Like Spectra among β Pic-Like Stars

1997 ◽  
Vol 161 ◽  
pp. 149-155 ◽  
Author(s):  
Harold M. Butner ◽  
Helen J. Walker ◽  
Diane H. Wooden ◽  
Fred C. Witteborn
Keyword(s):  
Main Sequence ◽  
Interplanetary Dust ◽  
Small Sample ◽  
Dust Particles ◽  
Striking Similarity ◽  
Early Solar System ◽  
Main Sequence Stars ◽  
Interplanetary Dust Particles ◽  
Mid Infrared ◽  
Physical Conditions

AbstractTo assess the physical conditions in our early solar system, we have to study the disks around other stars.βPic is a main sequence star surrounded by a large dust disk,βPic’s mid-infrared spectrum bears a striking resemblance to the silicate emission seen in some cometary spectra. We have selected a sample of main-sequence stars with similar IRAS properties to those ofβPic and undertaken a systematic survey of their physical properties. We obtained mid-infrared spectra covering the range 8 to 13μm at a resolution of 200 in June 1995. We report on the wide variety of silicate emission features we see and compare to the spectra reported for many different interstellar and interplanetary sources. Even among our small sample of stars, we find examples of silicate emission features that bear a striking similarity to those seen in the spectra of some comets like P/Halley and P/Bradfield 1987. These spectra also resemble the laboratory spectra of Interplanetary Dust Particles (IDPs).

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