Properties of interstellar wind leading to shape morphology  of the dust surrounding HD 61005

Pástor, P.

doi:10.1051/0004-6361/201730455

Cited by 3 publications

(3 citation statements)

References 40 publications

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“…This suggests that if the extended halo is indeed the consequence of interactions with the ISM gas, then, the dust grains would most likely be orbiting counter-clockwise around HR 4796 A. The main caveat in this scenario is the rather large density of the ISM gas required, compared to the surroundings of the solar system" similarly to what was found for HD 61005 by Pástor (2017). However, the volume density of the cold, dense, interstellar medium can vary between 5 − 100 cm −3 (e.g., Nguyen et al 2019 and references therein).…”

Section: Interaction With Local Ism Gasmentioning

confidence: 72%

“…The forces considered here are the gravitational potential from the central star (weighted by 1 − β when considering the effect of radiation pressure), and the gas drag on each dust grain. We followed the work of Marzari & Thébault (2011) (see also Pástor 2017) for the implementation, and the acceleration felt by a dust grain is estimated as…”

Section: Description Of the Codementioning

confidence: 99%

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Dust production in the debris disk around HR 4796 A

Olofsson

Milli

Thébault

et al. 2019

A&A

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Context. Debris disks are the natural by-products of the planet formation process. Scattered or polarized light observations are mostly sensitive to small dust grains that are released from the grinding down of bigger planetesimals. Aims. High angular resolution observations at optical wavelengths can provide key constraints on the radial and azimuthal distribution of the small dust grains. These constraints can help us better understand where most of the dust grains are released upon collisions. Methods. We present SPHERE/ZIMPOL observations of the debris disk around HR 4796 A, and model the radial profiles along several azimuthal angles of the disk with a code that accounts for the effect of stellar radiation pressure. This enables us to derive an appropriate description for the radial and azimuthal distribution of the small dust grains. Results. Even though we only model the radial profiles along (or close to) the semi-major axis of the disk, our best-fit model is not only in good agreement with our observations but also with previously published datasets (from near-IR to sub-mm wavelengths). We find that the reference radius is located at 76.4 ± 0.4 au, and the disk has an eccentricity of 0.076 +0.016 −0.010 , with the pericenter located on the front side of the disk (north of the star). We find that small dust grains must be preferentially released near the pericenter to explain the observed brightness asymmetry. Conclusions. Even though parent bodies spend more time near the apocenter, the brightness asymmetry implies that collisions happen more frequently near the pericenter of the disk. Our model can successfully reproduce the shape of the outer edge of the disk, without having to invoke an outer planet shepherding the debris disk. With a simple treatment of the effect of the radiation pressure, we conclude that the parent planetesimals are located in a narrow ring of about 3.6 au in width.

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Section: Interaction With Local Ism Gasmentioning

confidence: 72%

Section: Description Of the Codementioning

confidence: 99%

Dust production in the debris disk around HR 4796 A

Olofsson

Milli

Thébault

et al. 2019

A&A

View full text Add to dashboard Cite

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“…One mechanism that operates predominantly on small grains and that has been discussed extensively in the literature (e.g., Artymowicz & Clampin 1997;Debes et al 2009;Maness et al 2009;Pástor 2017) is interactions with the local interstellar medium (ISM), in which disk grains interact with gas in an ISM cloud, and are subsequently blown out due to gas drag or ram pressure stripping. Millimeter grains are not expected to feel a significant effect from interactions with the ISM.…”

Section: On the Origin Of The Millimeter Halo Componentmentioning

confidence: 99%

ALMA Detection of Extended Millimeter Halos in the HD 32297 and HD 61005 Debris Disks

MacGregor

Weinberger

Hughes

et al. 2018

ApJ

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We present ALMA 1.3 mm (230 GHz) observations of the HD 32297 and HD 61005 debris disks, two of the most iconic debris disks due to their dramatic swept-back wings seen in scattered light images. These observations achieve sensitivities of 14 and 13 µJy beam −1 for HD 32297 and HD 61005, respectively, and provide the highest resolution images of these two systems at millimeter wavelengths to date. By adopting a MCMC modeling approach, we determine that both disks are best described by a two-component model consisting of a broad (∆R/R > 0.4) planetesimal belt with a rising surface density gradient, and a steeply falling outer halo aligned with the scattered light disk. The inner and outer edges of the planetesimal belt are located at 78.5 ± 8.1 AU and 122 ± 3 AU for HD 32297, and 41.9 ± 0.9 AU and 67.0 ± 0.5 AU for HD 61005. The halos extend to 440 ± 32 AU and 188 ± 8 AU, respectively. We also detect 12 CO J= 2 − 1 gas emission from HD 32297 co-located with the dust continuum. These new ALMA images provide observational evidence that larger, millimeter-sized grains may also populate the extended halos of these two disks previously thought to only be composed of small, micron-sized grains. We discuss the implications of these results for potential shaping and sculpting mechanisms of asymmetric debris disks.

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The vertical structure of debris discs and the impact of gas

Olofsson

Thébault

Kral

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The vertical structure of debris disks provides clues about their dynamical evolution and the collision rate of the unseen planetesimals. Thanks to the ever-increasing angular resolution of contemporary instruments and facilities, we are beginning to constrain the scale height of a handful of debris disks, either at near-infrared or millimeter wavelengths. Nonetheless, this is often done for individual targets only. We present here the geometric modeling of eight disks close to edge-on, all observed with the same instrument (SPHERE) and using the same mode (dual-beam polarimetric imaging). Motivated by the presence of CO gas in two out of the eight disks, we then investigate the impact that gas can have on the scale height by performing N-body simulations including gas drag and collisions. We show that gas can quickly alter the dynamics of particles (both in the radial and vertical directions), otherwise governed by gravity and radiation pressure. We find that, in the presence of gas, particles smaller than a few tens of microns can efficiently settle toward the midplane at the same time as they migrate outward beyond the birth ring. For second generation gas (Mgas ≤ 0.1 M⊕), the vertical settling should be best observed in scattered light images compared to observations at millimeter wavelengths. But if the gas has a primordial origin (Mgas ≥ 1 M⊕), the disk will appear very flat both at near-infrared and sub-mm wavelengths. Finally, far beyond the birth ring, our results suggest that the surface brightness profile can be as shallow as ∼−2.25.

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Properties of interstellar wind leading to shape morphology of the dust surrounding HD 61005

Cited by 3 publications

References 40 publications

Dust production in the debris disk around HR 4796 A

Dust production in the debris disk around HR 4796 A

ALMA Detection of Extended Millimeter Halos in the HD 32297 and HD 61005 Debris Disks

The vertical structure of debris discs and the impact of gas

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