G. V. Ustyugova

Keldysh Institute of Applied Mathematics

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A. V. Koldoba

Moscow Institute of Physics and Technology

R. V. E. Lovelace

Cornell University

M. M. Romanova

Cornell University

M. M. Romanova

Cornell University

ВМ

В. М. Чечеткин

Keldysh Institute of Applied Mathematics

S. V. Bogovalov

Moscow Engineering Physics Institute

Patrick Lii

Cornell University

Sergei Dyda

University of Virginia

Min Long

University of South China

A. K. Kulkarni

ARC Centre of Excellence for Gravitational Wave Discovery

Cooperative Institutions

Cornell University

Keldysh Institute of Applied Mathematics

University of Milan

Moscow Engineering Physics Institute

California Institute of Technology

Center for Astrophysics Harvard & Smithsonian

Russian Academy of Sciences

University of Illinois Urbana-Champaign

Max Planck Society

Massachusetts Institute of Technology

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Modelling Interaction of Relativistic and Nonrelativistic Flows on Adaptive Grids

Mathematical Models and Computer Simulations (2019)

A. V. Koldoba G. V. Ustyugova S. V. Bogovalov

Dimensionless quantity

10.1134/s2070048219010095

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Citations (1)

The mathematical simulation of the magnetic field coronal loops evolution

T G Yelenina G. V. Ustyugova

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3D SIMULATIONS OF MAGNETOSPHERIC FLOW IN CLASSICAL T TAURI STARS. M.M. Romanova 1

R. V. E. Lovelace G. V. Ustyugova A. V. Koldoba

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The effect of an ordered azimuthal magnetic field on a migrating planet in a non-turbulent disc

arXiv (Cornell University) (2013)

M. L. Comins M. M. Romanova A. V. Koldoba G. V. Ustyugova R. V. E. Lovelace

In this work, we consider the physics of the interaction between a planet and a magnetized gaseous protoplanetary disc. We investigate the migration of a planet in a disc that is threaded with an azimuthal magnetic field. We find that, for a larger magnetic field amplitude, there is an increasingly large positive torque on the planet from the disc, resulting in slowed and even outward migration. Our results indicate that magnetic resonances due to a purely azimuthal, ordered magnetic field can slow or stop the inward migration of Jupiter-mass, Saturn-mass, and $5 M_{\oplus}$ planets.

10.48550/arxiv.1310.6697

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3D Simulations of Magnetospheric Flow in Classical T Tauri Stars

Protostars and Planets V Posters (2005)

M. M. Romanova R. V. E. Lovelace G. V. Ustyugova A. V. Koldoba

R.V.E. Lovelace, G.V. Ustyugova and A.V. Koldoba , 1 Space Science Building, Cornell University, Ithaca, NY 14853, Romanova@astro.cornell.edu , 2 Space Science Building, Cornell University, Ithaca, NY 14853, Lovelace@astro.cornell.edu, 3 Keldysh Institute of Applied Mathematics, Miusskaya sq. 4. , Moscow 125047, Russia, Ustyugg@rambler.ru , 4 Keldysh Institute of Applied Mathematics, Miusskaya sq. 4. , Moscow 125047, Russia, Koldoba@spp.Keldysh.ru

space science

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Eccentricity growth of massive planets inside cavities of protoplanetary discs

Monthly Notices of the Royal Astronomical Society (2023)

M. M. Romanova A. V. Koldoba G. V. Ustyugova Dong Lai R. V. E. Lovelace

ABSTRACT We carry out hydrodynamical simulations to study the eccentricity growth of a 1–30 Jupiter mass planet located inside the fixed cavity of a protoplanetary disc. The planet exchanges energy and angular momentum with the disc at resonant locations, and its eccentricity grows due to Lindblad resonances. We observe several phases of eccentricity growth where different eccentric Lindblad resonances dominate from 1:3 up to 3:5. The maximum values of eccentricity reached in our simulations are 0.65–0.75. We calculate the eccentricity growth rate for different planet masses and disc parameters and derive analytical dependencies on these parameters. We observe that the growth rate is proportional to both the planet’s mass and the characteristic disc mass for a wide range of parameters. In a separate set of simulations, we derived the width of the 1:3 Lindblad resonance.

Eccentricity (behavior)

Giant planet

Jupiter mass

10.1093/mnras/stad987

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Eccentricity and Inclination of Massive Planets Inside Low-density Cavities: Results of 3D Simulations

arXiv (Cornell University) (2024)

M. M. Romanova A. V. Koldoba G. V. Ustyugova Catherine Espaillat R. V. E. Lovelace

We study the evolution of eccentricity and inclination of massive planets in low-density cavities of protoplanetary discs using three-dimensional (3D) simulations. When the planet's orbit is aligned with the equatorial plane of the disc, the eccentricity increases to high values of 0.7-0.9 due to the resonant interaction with the inner parts of the disc. For planets on inclined orbits, the eccentricity increases due to the Kozai-Lidov mechanism, where the disc acts as an external massive body that perturbs the planet's orbit. At small inclination angles, < 30 degrees, the resonant interaction with the inner disc strongly contributes to the eccentricity growth, while at larger angles, eccentricity growth is mainly due to the Kozai-Lidov mechanism. We conclude that planets inside low-density cavities tend to acquire high eccentricity if favorable conditions give sufficient time for growth. The final value of the planet's eccentricity, after the disc dispersal depends on the planet's mass and properties of the cavity and protoplanetary disc.

Eccentricity (behavior)

10.48550/arxiv.2406.18834

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Formation of Stationary Magnetohydrodynamic Outflows from a Disk by Time‐dependent Simulations

The Astrophysical Journal (1997)

M. M. Romanova G. V. Ustyugova A. V. Koldoba В. М. Чечеткин R. V. E. Lovelace

We report the discovery of a family of stationary magnetohydrodynamic (MHD) outflows from a disk found by time-dependent, axisymmetric MHD simulations. The initial poloidal magnetic field threading the disk was taken to be a tapered monopole field, with the field strength on the disk decreasing outwardly to small values. At the disk surface, matter was given a small initial push with a speed less than the slow magnetosonic speed. In the simulations, the outflowing matter is observed to be accelerated by magnetic and centrifugal forces up to velocities in excess of the fast magnetosonic speed and in excess of the escape speed.

10.1086/304199

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Citations (86)

One-sided outflows/jets from rotating stars with complex magnetic fields

Monthly Notices of the Royal Astronomical Society (2010)

R. V. E. Lovelace M. M. Romanova G. V. Ustyugova A. V. Koldoba

We investigate the generation of intrinsically asymmetric or {\it one-sided} outflows or jets from disk accretion onto rotating stars with complex magnetic fields using axisymmetric (2.5D) magnetohydrodynamic simulations. The intrinsic magnetic field of the star is assumed to consist of a superposition of an aligned dipole and an aligned quadrupole in different proportions. The star is assumed to be rapidly rotating in the sense that the star's magnetosphere is in the propeller regime where strong outflows occur. Our simulations show that for conditions where there is a significant quadrupole component in addition to the dipole component, then a dominantly {\it one-sided} conical wind tends to form on the side of the equatorial plane with the larger value of the intrinsic axial magnetic field at a given distance. For cases where the quadrupole component is absent or very small, we find that dominantly one-sided outflows also form, but the direction of the flow "flip-flops" between upward and downward on a time-scale of $\sim 30$ days for a protostar. The average outflow will thus be symmetrical. In the case of a pure quadrupole field we find symmetric outflows in the upward and downward directions.

Outflow

Protostar

10.1111/j.1365-2966.2010.17284.x

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Citations (46)

Numerical simulations of coronal magnetic field loop evolution

arXiv (Cornell University) (2006)

T G Yelenina G. V. Ustyugova A. V. Koldoba

We present the results of the numerical simulations of the interaction between a magnetized star and an imperfectly conducting accretion disk. To analyze the ''star-disk'' interaction we numerically investigate the MHD equations used Godunov-type high resolution numerical method. It was found that the ''star-disk'' interaction occurs with quasi-periodic reconnection of the magnetic field coronal loops and plasmoid ejections. In the case of the perfect disk conductivity the evolution of the coronal magnetic field leads to the periodic outflow of angular momentum from the disk. In the case of an imperfectly conducting disk the configuration of the magnetic field is formed such that the disk angular momentum carried by magnetic field gets balanced by angular momentum carried by matter.

Coronal loop

10.48550/arxiv.astro-ph/0603857

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