Modeling circumstellar disc fragmentation and episodic protostellar accretion with smoothed particle hydrodynamics in cell

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Modeling circumstellar disc fragmentation and episodic protostellar accretion with smoothed particle hydrodynamics in cell. / Stoyanovskaya, O. P.; Snytnikov, N. V.; Snytnikov, V. N.

In: Astronomy and Computing, Vol. 21, 01.10.2017, p. 1-14.

Research output: Contribution to journal › Article › peer-review

BibTeX

@article{411662455b6142a1b6bf22066ec2c2f4,

title = "Modeling circumstellar disc fragmentation and episodic protostellar accretion with smoothed particle hydrodynamics in cell",

abstract = "We discuss the ability of the smoothed particle hydrodynamics (SPH) method combined with a grid-based solver for the Poisson equation to model mass accretion onto protostars in gravitationally unstable protostellar discs. We scrutinize important features of coupling the SPH with grid-based solvers and numerical issues associated with (1) large number of SPH neighbors and (2) relation between gravitational softening and hydrodynamic smoothing length. We report results of our simulations of razor-thin disc prone to fragmentation and demonstrate that the algorithm being simple and homogeneous captures the target physical processes — disc gravitational fragmentation and accretion of gas onto the protostar caused by inward migration of dense clumps. In particular, we obtain two types of accretion bursts: a short-duration one caused by a quick inward migration of the clump, previously reported in the literature, and the prolonged one caused by the clump lingering at radial distances on the order of 15–25 au. The latter is culminated with a sharp accretion surge caused by the clump ultimately falling on the protostar.",

keywords = "Hydrodynamics, Instabilities, Protoplanetary discs, RESOLUTION, BURST MODE, PLANET FORMATION, SELF-GRAVITATING DISCS, FU-ORIONIS, CONVERGENCE, STARS, PROTOPLANETARY DISCS, SIMULATIONS, THERMAL ENERGETICS",

author = "Stoyanovskaya, {O. P.} and Snytnikov, {N. V.} and Snytnikov, {V. N.}",

note = "Publisher Copyright: {\textcopyright} 2017 Elsevier B.V.",

year = "2017",

month = oct,

day = "1",

doi = "10.1016/j.ascom.2017.09.001",

language = "English",

volume = "21",

pages = "1--14",

journal = "Astronomy and Computing",

issn = "2213-1337",

publisher = "Elsevier",

}

RIS

TY - JOUR

T1 - Modeling circumstellar disc fragmentation and episodic protostellar accretion with smoothed particle hydrodynamics in cell

AU - Stoyanovskaya, O. P.

AU - Snytnikov, N. V.

AU - Snytnikov, V. N.

PY - 2017/10/1

Y1 - 2017/10/1

N2 - We discuss the ability of the smoothed particle hydrodynamics (SPH) method combined with a grid-based solver for the Poisson equation to model mass accretion onto protostars in gravitationally unstable protostellar discs. We scrutinize important features of coupling the SPH with grid-based solvers and numerical issues associated with (1) large number of SPH neighbors and (2) relation between gravitational softening and hydrodynamic smoothing length. We report results of our simulations of razor-thin disc prone to fragmentation and demonstrate that the algorithm being simple and homogeneous captures the target physical processes — disc gravitational fragmentation and accretion of gas onto the protostar caused by inward migration of dense clumps. In particular, we obtain two types of accretion bursts: a short-duration one caused by a quick inward migration of the clump, previously reported in the literature, and the prolonged one caused by the clump lingering at radial distances on the order of 15–25 au. The latter is culminated with a sharp accretion surge caused by the clump ultimately falling on the protostar.

AB - We discuss the ability of the smoothed particle hydrodynamics (SPH) method combined with a grid-based solver for the Poisson equation to model mass accretion onto protostars in gravitationally unstable protostellar discs. We scrutinize important features of coupling the SPH with grid-based solvers and numerical issues associated with (1) large number of SPH neighbors and (2) relation between gravitational softening and hydrodynamic smoothing length. We report results of our simulations of razor-thin disc prone to fragmentation and demonstrate that the algorithm being simple and homogeneous captures the target physical processes — disc gravitational fragmentation and accretion of gas onto the protostar caused by inward migration of dense clumps. In particular, we obtain two types of accretion bursts: a short-duration one caused by a quick inward migration of the clump, previously reported in the literature, and the prolonged one caused by the clump lingering at radial distances on the order of 15–25 au. The latter is culminated with a sharp accretion surge caused by the clump ultimately falling on the protostar.

KW - Hydrodynamics

KW - Instabilities

KW - Protoplanetary discs

KW - RESOLUTION

KW - BURST MODE

KW - PLANET FORMATION

KW - SELF-GRAVITATING DISCS

KW - FU-ORIONIS

KW - CONVERGENCE

KW - STARS

KW - PROTOPLANETARY DISCS

KW - SIMULATIONS

KW - THERMAL ENERGETICS

UR - http://www.scopus.com/inward/record.url?scp=85030682928&partnerID=8YFLogxK

U2 - 10.1016/j.ascom.2017.09.001

DO - 10.1016/j.ascom.2017.09.001

M3 - Article

AN - SCOPUS:85030682928

VL - 21

SP - 1

EP - 14

JO - Astronomy and Computing

JF - Astronomy and Computing

SN - 2213-1337

ER -

ID: 9078941