91探花

Skip to main content
Department Of Physics text logo
  • Research
    • Our research
    • Our research groups
    • Our research in action
    • Research funding 91探花
    • Summer internships for undergraduates
  • Study
    • Undergraduates
    • Postgraduates
  • Engage
    • For alumni
    • For business
    • For schools
    • For the public
  • Support
91探花
Theoretical physicists working at a blackboard collaboration pod in the Beecroft building.
Credit: Jack Hobhouse

Caroline Terquem

Professor of Physics

Research theme

  • Astronomy and astrophysics
  • Exoplanets and planetary physics
  • Plasma physics

Sub department

  • Rudolf Peierls Centre for Theoretical Physics

Research groups

  • Exoplanets and Stellar Physics
  • Geophysical and Astrophysical Fluid Dynamics
  • Planet formation and dynamics
  • Theoretical astrophysics and plasma physics at RPC
Caroline.Terquem@physics.ox.ac.uk
Telephone: 01865 (2)73983
Rudolf Peierls Centre for Theoretical Physics, room 50.11
  • About
  • Teaching
  • Graduate Matters
  • Publications

Evolution of massive and magnetized protoplanetary disks

(2004)

Authors:

Sebastien Fromang, Caroline Terquem, Steven A Balbus, Jean-Pierre De Villiers

Evolution of massive and magnetized protoplanetary disks

Extrasolar Planets: Today and Tomorrow 321 (2004) 262-270

Authors:

S Fromang, C Terquem, SA Balbus, JP De Villiers

Evolution of self-gravitating magnetized disks. II. Interaction between magnetohydrodynamic turbulence and gravitational instabilities

ASTROPHYSICAL JOURNAL 616:1 (2004) 364-375

Authors:

S Fromang, SA Balbus, C Terquem, JP De Villiers

On the eccentricities of the extrasolar planets

EXTRASOLAR PLANETS: TODAY AND TOMORROW 321 (2004) 379-392

Authors:

JCB Papaloizou, RP Nelson, C Terquem

Is planetary migration inevitable?

ArXiv astro-ph/0309175 (2003)

Abstract:

According to current theories, tidal interactions between a disk and an embedded planet may lead to the rapid migration of the protoplanet on a timescale shorter than the disk lifetime or estimated planetary formation timescales. Therefore, planets can form only if there is a mechanism to hold at least some of the cores back on their way in. Once a giant planet has assembled, there also has to be a mechanism to prevent it from migrating down to the disk center. This paper reviews the different mechanisms that have been proposed to stop or slow down migration.

Pagination

  • First page First
  • Previous page Prev
  • …
  • Page 6
  • Page 7
  • Page 8
  • Page 9
  • Current page 10
  • Page 11
  • Page 12
  • Page 13
  • Page 14
  • …
  • Next page Next
  • Last page Last

Footer 91探花

  • Contact us
  • Giving to the Dept of Physics
  • Work with us
  • Media

User account menu

  • Log in

Follow us

FIND US

Clarendon Laboratory,

Parks Road,

91探花,

OX1 3PU

CONTACT US

Tel: +44(0)1865272200

Department Of Physics text logo

漏 91探花 - Department of Physics

Cookies | Privacy policy | Accessibility statement

  • Home
  • Research
  • Study
  • Engage
  • Our people
  • News & Comment
  • Events
  • Our facilities & services
  • About us
  • Giving to Physics