Disk Frequencies and Lifetimes in Young Clusters

Haisch, Karl E.; Lada, Elizabeth A.; Lada, Charles J.

doi:10.1086/320685

Cited by 1,664 publications

(1,774 citation statements)

References 34 publications

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“…We showed that an important consequence of including these effects is to drastically reduce the formation timescale (Alibert et al 2004) bringing it to an excellent agreement with the observationally derived lifetime of proto-planetary disks (Haisch et al 2001). The numerical tools we have developed, as well as the tests we have performed to validate them can be found in Alibert et al (2005a).…”

Section: Giant Planet Formation Modelsupporting

confidence: 61%

Exoplanets: The tip of the iceberg?

et al. 2005

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Abstract. As the number of large scale ground-and space-bound planet detection and imaging projects is growing, the need for theoretical guidance in order to optimize instrumental design is rapidly mounting. In an effort to provide this required framework, we present the results of Monte Carlo simulations of the formation of giant planets and compare them with the current population of exoplanets. Our models show that due to the severe current observational detection bias only a small percentage (3.6 %) of the potentially existing planets can be detected. Indeed, a large number of planetary embryos never grow enough to become giant planets giving raise to a large populations of bodies with masses smaller than 5 M jup . In addition, this observational bias, coupled with the fact that systems enriched in heavy elements tend to form more massive planets, explains the currently observed correlation between stellar metallicity and likelihood to host planets. Finally, we show that the disk gas delivery rate during the late stages of formation actually determines the maximum planetary mass.

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Section: Giant Planet Formation Modelsupporting

confidence: 61%

Exoplanets: The tip of the iceberg?

et al. 2005

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“…Proper motions also provided membership information and a number of proto-planetary disk-bearing stars were revealed, yielding a disk fraction of 6% (Stolte et al 2010), similar to other massive young clusters throughout the Milky Way (e.g. Haisch et al 2001;Stolte et al 2006;Hernández et al 2007;Harayama et al 2008). This low disk fraction at 2.5 Myr shows that proto-planetary disk evolution, and possibly planet formation, are strongly modified in the environment of a massive cluster.…”

Section: The Arches and Quintuplet Clustersmentioning

confidence: 66%

Young stars in the Galactic center

Lu¹,

Ghez

Morris

et al. 2013

Proc. IAU

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Abstract. The central parsec of our Galaxy hosts not only a supermassive black hole, but also a large population of young stars (age <6 Myr) whose presence is puzzling given how inhospitable the region is for star formation. The strong tidal forces require gas densities many orders of magnitude higher than is found in typical molecular clouds. Kinematic observations of this young nuclear cluster show complex structures, including a well-defined inner disk, but also a substantial off-disk population. Spectroscopic and photometric measurements indicate the initial mass function (IMF) differs significantly from the canonical IMF found in the solar neighborhood. These observations have led to a number of proposed star formation scenarios, such as an infalling massive star cluster, a single infalling molecular cloud, or cloud-cloud collisions. I will review recent works on the young stars in the central parsec and discuss connections with young nuclear star clusters in other galaxies, such as M31, and with star formation in the larger central molecular zone.

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“…For an unmagnetized disk, Tanaka et al (2002) showed that the protoplanet of 5M ⊕ located at 5AU and embedded in the minimum-mass solar nebula (Hayashi et al 1985) migrates inward in 8×10 5 years, which is shorter than the observed lifetime of a protoplanetary disk [∼ 10 7 years, see e.g., Haisch et al 2001].…”

Section: Introductionmentioning

confidence: 99%

The effect of poloidal magnetic field on type I planetary migration

Muto¹,

Machida²,

Inutsuka³

2007

Proc. IAU

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Abstract.We study the effect of poloidal magnetic field on type I planetary migration by linear perturbation analysis with the shearing-sheet approximation and the analytic results are compared with numerical calculation. We investigate the cases where magneto-rotational instability (MRI) does not occur: either the disk is two-dimensional, or a very strong field is exerted. We derive formulae for torque exerted on the planet for both cases. We find that twodimensional torque is suppressed when plasma beta is less than 1 and three-dimensional modes dominate, in contrast to unmagnetized case.

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Disk Frequencies and Lifetimes in Young Clusters

Cited by 1,664 publications

References 34 publications

Exoplanets: The tip of the iceberg?

Exoplanets: The tip of the iceberg?

Young stars in the Galactic center

The effect of poloidal magnetic field on type I planetary migration

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