Circumstellar Disks

Beckwith, S.

doi:10.1007/978-94-011-4509-1_17

Cited by 38 publications

(13 citation statements)

References 65 publications

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“…During the epoch of their formation, protoplanets are embedded in protostellar disks that have been found around most young stellar objects (Haisch, Lada, & Lada 2001). The mass and temperature distribution of these disks are very similar to those inferred from the minimum mass nebula model for the solar system (Beckwith 1999). The self-gravity of these disks can induce the orbits of planets formed within them to precess at a rate faster than that due to their mutual perturbation.…”

Section: Introductionmentioning

confidence: 56%

Eccentricity Evolution of Extrasolar Multiple Planetary Systems Due to the Depletion of Nascent Protostellar Disks

Nagasawa¹,

Lin²,

Ida³

2003

ApJ

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Most extrasolar planets are observed to have eccentricities much larger than those in the solar system. Some of these planets have sibling planets, with comparable masses, orbiting around the same host stars. In these multiple planetary systems, eccentricity is modulated by the planets' mutual secular interaction as a consequence of angular momentum exchange between them. For mature planets, the eigenfrequencies of this modulation are determined by their mass and semimajor axis ratios. However, prior to the disk depletion, self-gravity of the planets' nascent disks dominates the precession eigenfrequencies. We examine here the initial evolution of young planets' eccentricity due to the apsidal libration or circulation induced by both the secular interaction between them and the self-gravity of their nascent disks. We show that as the latter effect declines adiabatically with disk depletion, the modulation amplitude of the planets' relative phase of periapsis is approximately invariant despite the time-asymmetrical exchange of angular momentum between planets. However, as the young planets' orbits pass through a state of secular resonance, their mean eccentricities undergo systematic quantitative changes. For applications, we analyze the eccentricity evolution of planets around Andromedae and HD 168443 during the epoch of protostellar disk depletion. We find that the disk depletion can change the planets' eccentricity ratio. However, the relatively large amplitude of the planets' eccentricity cannot be excited if all the planets had small initial eccentricities.

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Section: Introductionmentioning

confidence: 56%

Eccentricity Evolution of Extrasolar Multiple Planetary Systems Due to the Depletion of Nascent Protostellar Disks

Nagasawa¹,

Lin²,

Ida³

2003

ApJ

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“…Infrared and submillimeter observations of T Tauri stars in dark clouds show that roughly half are orbited by an optically thick circumstellar dust disk (see review by Beckwith 1999). While the stars in our sample are roughly an order of magnitude older ($30 Myr) than typical T Tauri stars in dark clouds ( 3 Myr), we can ask the question: If the Tuc-Hor stars have optically thick, geometrically thin disks, what is the minimum inner hole radius allowed by observations?…”

Section: Optically Thick Disk With Inner Holementioning

confidence: 99%

Constraining the Lifetime of Circumstellar Disks in the Terrestrial Planet Zone: A Mid‐Infrared Survey of the 30 Myr old Tucana‐Horologium Association

Mamajek¹,

Meyer²,

Hinz³

et al. 2004

ApJ

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We have conducted an N-band survey of 14 young stars in the $30 Myr old Tucana-Horologium association to search for evidence of warm, circumstellar dust disks. Using the MIRAC-BLINC camera on the Magellan I (Baade) 6.5 m telescope, we find that none of the stars have a statistically significant N-band excess compared to the predicted stellar photospheric flux. Using three different sets of assumptions, this null result rules out the existence of the following around these post-T Tauri stars: (1) optically thick disks with inner hole radii of P0.1 AU, (2) optically thin disks with masses of less than 10 À6 M È (in $1 m sized grains) within P10 AU of these stars, and (3) scaled-up analogs of the solar system zodiacal dust cloud with more than 4000 times the emitting area. Our survey was sensitive to dust disks in the terrestrial planet zone with fractional luminosity of log (L dust =L Ã ) $10 À2:9 , yet none were found. Combined with results from previous surveys, these data suggest that circumstellar dust disks become so optically thin as to be undetectable at N band before age $20 Myr. We also present N-band photometry for several members of other young associations and a subsample of targets that will be observed with

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“…Photometric observations from 3.6-160µm probe temperatures (radii) encompassing the entire system of planets in our solar system [2]. Detailed spectrophotometry from 5.3-40 µm will permit a search for gaps in disks caused by the dynamical interaction of young gas giant planets and the particulate disk from 0.2-10 AU [3].…”

Section: Formation Of Planetary Embryosmentioning

confidence: 99%

The Formation and Evolution of Planetary Systems: SIRTF Legacy Science in the VLT Era

Meyer

Backman

Beckwith³

et al. 2002

The Origins of Stars and Planets: The VLT View

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Abstract. We will utilize the sensitivity of SIRTF through the Legacy Science Program to carry out spectrophotometric observations of solar-type stars aimed at (1) defining the timescales over which terrestrial and gas giant planets are built, from measurements diagnostic of dust/gas masses and radial distributions; and (2) establishing the diversity of planetary architectures and the frequency of planetesimal collisions as a function of time through observations of circumstellar debris disks. Together, these observations will provide an astronomical context for understanding whether our solar system -and its habitable planet -is a common or a rare circumstance.Achieving our science goals requires measuring precise spectral energy distributions for a statistically robust sample capable of revealing evolutionary trends and the diversity of system outcomes. Our targets have been selected from two carefully assembled databases of solar-like stars: (1) a sample located within 50 pc of the Sun spanning an age range from 100-3000 Myr for which a rich set of ancillary measurements (e.g. metallicity, stellar activity, kinematics) are available; and (2) a selection located between 15 and 180 pc and spanning ages from 3 to 100 Myr. For stars at these distances SIRTF is capable of detecting stellar photospheres with SNR >30 at λ ≤ 24µm for our entire sample, as well as achieving SNR >5 at the photospheric limit for over 50% of our sample at λ = 70µm. Thus we will provide a complete census of stars with excess emission down to the level produced by the dust in our present-day solar system. SIRTF observations obtained as part of this program will provide a rich Legacy for follow-up observations utilizing a variety of facilities including the VLT. More information concerning our program can be found at http://gould.as.arizona.edu/feps.

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Circumstellar Disks

Cited by 38 publications

References 65 publications

Eccentricity Evolution of Extrasolar Multiple Planetary Systems Due to the Depletion of Nascent Protostellar Disks

Eccentricity Evolution of Extrasolar Multiple Planetary Systems Due to the Depletion of Nascent Protostellar Disks

Constraining the Lifetime of Circumstellar Disks in the Terrestrial Planet Zone: A Mid‐Infrared Survey of the 30 Myr old Tucana‐Horologium Association

The Formation and Evolution of Planetary Systems: SIRTF Legacy Science in the VLT Era

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