I
am a Professor in the Department of Astronomy of Yale University.
EDUCATION:
I was educated in India and held postdoctoral positions in Queen Mary College, London, U.K. and the Theoretical Astrophysics Centre (TAC) at the University of Aarhus, Denmark before moving to the U.S. to become a member of the Institute for Advanced Study in Princeton. I joined Yale in 2000.
RESEARCH:
My research interests include the study of the Sun and stars, and using these to study properties of stellar matter. Highlights of current and past research can be found in my Research page.
I use the techniques of helioseismology to study the Sun. My current interest is to study solar-cycle related changes in the Sun. I use data from the Global Oscillation Network Group (GONG) as well as the Michelson Doppler Imager (MDI) on SOHO. I am a Co-I of the upcoming Solar Dynamics Observatory (SDO), and hope to use data from the Helioseismic and Magnetic Imager (HMI) on board SDO once SDO is launched and working.
My past solar research involved determining the details of the internal structure and dynamics of the Sun. I successfully determined the precise position of the base of the solar convection zone as well the helium abundance of the Sun. I have also studied the equation of state of solar matter. Even before the results from the Sudbury Neutrino Observatory were published, our results had shown that the solution of the solar neutrino problem must lie with particle physics and that the problem was not caused by deficiencies in our models of the Sun. I have also been working on the helioseismic determination of solar metallicity, a review of my abundance work can be seen here.
My stellar physics research involves both theoretical studies and the use of asteroseismology. I am a member of the Kepler Asteroseismic Science Consortium (KASC), asteroseismic data obtained by Kepler will allow us to study the details of stars in a manner that has not been possible so far.
Another area of research that I am currently involved in is the study of convective heat transport in stars. Convection remains the most uncertain ingredient in stellar modelling, however with current computers it is possible to simulate convective heat transport in the outer layers of stars. My group has recently begun a large-scale study of stellar convection across a large part of the HR diagram.
EDUCATION:
I was educated in India and held postdoctoral positions in Queen Mary College, London, U.K. and the Theoretical Astrophysics Centre (TAC) at the University of Aarhus, Denmark before moving to the U.S. to become a member of the Institute for Advanced Study in Princeton. I joined Yale in 2000.
RESEARCH:
My research interests include the study of the Sun and stars, and using these to study properties of stellar matter. Highlights of current and past research can be found in my Research page.
I use the techniques of helioseismology to study the Sun. My current interest is to study solar-cycle related changes in the Sun. I use data from the Global Oscillation Network Group (GONG) as well as the Michelson Doppler Imager (MDI) on SOHO. I am a Co-I of the upcoming Solar Dynamics Observatory (SDO), and hope to use data from the Helioseismic and Magnetic Imager (HMI) on board SDO once SDO is launched and working.
My past solar research involved determining the details of the internal structure and dynamics of the Sun. I successfully determined the precise position of the base of the solar convection zone as well the helium abundance of the Sun. I have also studied the equation of state of solar matter. Even before the results from the Sudbury Neutrino Observatory were published, our results had shown that the solution of the solar neutrino problem must lie with particle physics and that the problem was not caused by deficiencies in our models of the Sun. I have also been working on the helioseismic determination of solar metallicity, a review of my abundance work can be seen here.
My stellar physics research involves both theoretical studies and the use of asteroseismology. I am a member of the Kepler Asteroseismic Science Consortium (KASC), asteroseismic data obtained by Kepler will allow us to study the details of stars in a manner that has not been possible so far.
Another area of research that I am currently involved in is the study of convective heat transport in stars. Convection remains the most uncertain ingredient in stellar modelling, however with current computers it is possible to simulate convective heat transport in the outer layers of stars. My group has recently begun a large-scale study of stellar convection across a large part of the HR diagram.
Postal
address:
Astronomy Dept.
P.O. Box 208101
New Haven,
CT 06520-8101
USA
Express
mail:
Astronomy
Dept.
260
Whitney Avenue
New
Haven, CT 06511
U.S.A
-
Phone: (+1) 203 432 3028
Fax: (+1) 203 432 5048
E-mail:
sarbani.basu @ yale.edu