Marina M. Romanova is a Russian-American computational astrophysicist, known for her work simulating the magnetohydrodynamics of accretion disks, including their interactions with the stellar magnetic fields of T Tauri stars and other young magnetized stars,[1] and the formation of magnetic towers along the rotation axis of the accretion disks of black holes.[2] She works as a senior research associate in the Cornell Center for Astrophysics and Planetary Science, in the Department of Astronomy at Cornell University.[3]

Education and career

Romanova studied astronomy at Moscow State University, graduating in 1978. After continuing as a graduate student at Moscow State University, she became a researcher at the Russian Space Research Institute from 1981 to 1996, earning a Ph.D. in astrophysics and radioastronomy there in 1986 under the joint supervision of Yakov Zeldovich and Gennady S. Bisnovatyi-Kogan.[4]

She came to Cornell University as a visiting scientist in 1996, and became a permanent researcher there in 1999.[4]

References

  1. ↑ "Numerical Investigation of Young Stars", Image gallery, NASA High-End Computing Program, retrieved 2023-01-16
  2. ↑ Meier, David L. (2012), Black Hole Astrophysics: The Engine Paradigm, Springer Praxis Books, Springer Science & Business Media, p. 650, Bibcode:2012bhae.book.....M, ISBN 9783642019364
  3. ↑ Marina Romanova, Cornell Department of Astronomy, retrieved 2023-01-16
  4. 1 2 Curriculum vitae, Cornell Department of Astronomy, retrieved 2023-01-16
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