Summary
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 edit
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 edit
- ^ "Numerical Investigation of Young Stars", Image gallery, NASA High-End Computing Program, retrieved 2023-01-16
- ^ 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
- ^ Marina Romanova, Cornell Department of Astronomy, retrieved 2023-01-16
- ^ a b Curriculum vitae, Cornell Department of Astronomy, retrieved 2023-01-16
External links edit
- Home page
- Marina Romanova publications indexed by Google Scholar