Vladimir S. Airapetian

3D Global Coronal Density Structure and Associated Magnetic Field near Solar Maximum

Measurement of the coronal magnetic field is a crucial ingredient in understanding the nature of solar coronal dynamic phenomena at all scales. We employ STEREO/COR1 data obtained near maximum of solar activity in December 2012 (Carrington rotation, CR 2131) to retrieve and analyze the three-dimensional (3D) coronal electron density in the range of heights from

Weighing supermassive black holes with the UV photon sieve space telescope

1.5

The Origins Space Telescope: Towards An Understanding of Temperate Planetary Atmospheres

to

The continued importance of habitability studies

4\ \mathrm{R}_\odot

Life Beyond the Solar System: Observation and Modeling of Exoplanet Environments

using a tomography method and qualitatively deduce structures of the coronal magnetic field. The 3D electron density analysis is complemented by the 3D STEREO/EUVI emissivity in 195 A\ band obtained by tomography for the same CR period. We find that the magnetic field configuration during CR 2131 has a tendency to become radially open at heliocentric distances below

Exoplanet Science Priorities from the Perspective of Internal and Surface Processes for Silicate and Ice Dominated Worlds.

\sim 2.5 \ \mathrm{R}_\odot

Atmospheric Heating and Wind Acceleration: Results for Cool Evolved Stars based on Proposed Processes

. We compared the reconstructed 3D coronal structures over the CR near the solar maximum to the one at deep solar minimum. Results of our 3D density reconstruction will help to constrain solar coronal field models and test the accuracy of the magnetic field approximations for coronal modeling.

Stellar Imager (SI): developing and testing a predictive dynamo model for the Sun by imaging other stars

The Photon Sieve Space Telescope (PSST) is a space-based ultra high-resolution (5 mas) narrow band (λ/Δλ ≃ 1000) spectral UV imager providing spectral imaging of astronomical objects in Ly - ∝, CIV and NV emission lines. Science obtained with this telescope will revolutionize our understanding of a whole range of astrophysical processes in the local and distant universe. There will be a dramatic increase in the number of observed moderate and large SMBH masses as well as extra-solar protoplanetary disks. The observations will also enable tracing the star formation rates in active galaxies. We present the optical design, the properties and the future implementation of the proposed UV photon sieve space telescope.