Effects of photophoresis on the evolution of transitional circumstellar disks

Herrmann, F.; Krivov, A. V.

doi:10.1051/0004-6361:20078322

Cited by 24 publications

(20 citation statements)

References 68 publications

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“…• Particle radius a • Thermal conductivity of the particle λ P So far, work on photophoresis in protoplanetary disks has considered the force imposed on particles by stellar radiation and in the midplane of protoplanetary disks (Krauss and Wurm 2005;Krauss et al 2007;Mousis et al 2007;Wurm 2007;Herrmann and Krivov 2008;Takeuchi and Krauss 2008). This is restricted to disk configurations where stellar radiation illuminates the particles and is important at the inner edge of the disk and at (late) times when the disk overall has become transparent.…”

Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

Outward transport of CAIs during FU‐Orionis events

Wurm¹,

Haack

2009

Meteorit & Planetary Scien

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available online at http://meteoritics.org Abstract-Evidence from meteorites shows that the first solids to form in the solar system, calciumaluminum-rich inclusions (CAIs), were transported outward from the Sun by several AU in the early solar system. We introduce a new concept of levitation and outward transport of CAIs at the surface of protoplanetary disks. Thermal radiation from the disk and the Sun can cause particles to levitate above the disk and drift outward through a process known as photophoresis. During normal conditions this process only works for dust-sized particles but during high luminosity events like FU-Orionis Outward transport of CAIs during FU-Orionis events

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Section: Levitation By Photophoresis Based On Thermal Radiationmentioning

confidence: 99%

Outward transport of CAIs during FU‐Orionis events

Wurm¹,

Haack

2009

Meteorit & Planetary Scien

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“…Note that additional radial forces such as photophoresis (Herrmann & Krivov 2007) can be included by simply adding them to the left part of Eq. (17).…”

Section: Radial Dynamics Of Dust Under Photogravity and Gas Dragmentioning

confidence: 99%

“…For a thermally-supported gas disk, we follow a standard description of the dust aerodynamics (Weidenschilling 1977), generalized to the presence of radiation pressure (Takeuchi & Artymowicz 2001;Thébault & Augereau 2005;Herrmann & Krivov 2007). The factor η is…”

Section: Gas Dragmentioning

confidence: 99%

Can gas in young debris disks be constrained by their radial brightness profiles?

Krivov¹,

Herrmann²,

Brandeker

et al. 2009

A&A

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Disks around young stars are known to evolve from optically thick, gas-dominated protoplanetary disks to optically thin, almost gasfree debris disks. It is thought that the primordial gas is largely removed at ages of ∼10 Myr and indeed, only little amounts of gas have been deduced from observations for debris disks at ages of > ∼ 10 Myr. However, gas detections are difficult and often indirect, not allowing one to discern the true gas densities. This suggests using dynamical arguments: it has been argued that gas, if present with higher densities, would lead to flatter radial profiles of the dust density and brightness than those actually observed. In this paper, we systematically study the influence of gas on the radial profiles of brightness. We assume that dust is replenished by planetesimals orbiting in a "birth ring" and model the dust distribution and scattered-light brightness profile in the outer part of the disk exterior to the birth ring, under different assumptions about the gas component. Our numerical simulations, supported with an analytic model, show that the radial profile of dust density and the surface brightness are surprisingly insensitive to variation of the parameters of a central star, location of the dust-producing planetesimal belt, dustiness of the disk and -most importantly -the parameters of the ambient gas. The radial brightness slopes in the outer disks are all typically in the range −3...−4. This result holds for a wide range of gas densities (three orders of magnitude), for different radial profiles of the gas temperature, both for gas of solar composition and gas of strongly non-solar composition. The slopes of −3...−4 we find are the same that were theoretically found for gas-free debris disks, and they are the same as actually retrieved from observations of many debris disks. Our specific results for three young (10−30 Myr old), spatially resolved, edge-on debris disks (β Pic, HD 32297, and AU Mic) show that the observed radial profiles of the surface brightness do not pose any stringent constraints on the gas component of the disk. We cannot exclude that outer parts of the systems may have retained substantial amounts of primordial gas which is not evident in the gas observations (e.g. as much as 50 Earth masses for β Pic). However, the possibility that gas, most likely secondary, is only present in little to moderate amounts, as deduced from gas detections (e.g. ∼0.05 Earth masses in the β Pic disk or even less), remains open, too.

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“…In some circumstances, photophoresis 3 drives small particles radially outward through an optically thin gaseous disk (e.g., Krauss & Wurm 2005;Herrmann & Krivov 2007;Cuello et al 2016). When photophoresis is effective, the time scale for radial drift is comparable to (and sometimes shorter than) the time scale for radial drift due to gas drag.…”

Section: Neat Planet Formation In a Remnant Gas Diskmentioning

confidence: 99%

Rocky Planet Formation: Quick and Neat

Kenyon

Najita

Bromley

2016

ApJ

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We reconsider the commonly held assumption that warm debris disks are tracers of terrestrial planet formation. The high occurrence rate inferred for Earthmass planets around mature solar-type stars based on exoplanet surveys (∼ 20%) stands in stark contrast to the low incidence rate (≤ 2%-3%) of warm dusty debris around solar-type stars during the expected epoch of terrestrial planet assembly (∼ 10 Myr). If Earth-mass planets at AU distances are a common outcome of the planet formation process, this discrepancy suggests that rocky planet formation occurs more quickly and/or is much neater than traditionally believed, leaving behind little in the way of a dust signature. Alternatively, the incidence rate of terrestrial planets has been overestimated or some previously unrecognized physical mechanism removes warm dust efficiently from the terrestrial planet region. A promising removal mechanism is gas drag in a residual gaseous disk with a surface density 10 −5 of the minimum mass solar nebula.

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Effects of photophoresis on the evolution of transitional circumstellar disks

Cited by 24 publications

References 68 publications

Outward transport of CAIs during FU‐Orionis events

Outward transport of CAIs during FU‐Orionis events

Can gas in young debris disks be constrained by their radial brightness profiles?

Rocky Planet Formation: Quick and Neat

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