Welcome to our website. If you are wondering what do the beautiful images from the home page collage convey, then you have come to the right spot.
Here is a list.
1.
From Prof Katia Ferriere, shows a schematic for Faraday rotation.
Shown qualitatively how the electric field vector of a linearly polarized radio wave oscillates along the propagation direction, between the source (far side) and the observer (near side), and how the polarization orientation (red double-headed arrow) undergoes Faraday rotation as the wave passes through a magneto-ionized region (blue shaded region).13 Faraday rotation is always right-handed about the magnetic field, B⃗ . When B⃗ points toward (away from) the observer, Faraday rotation is counterclockwise (clockwise) in the plane of the sky; this corresponds to a positive (negative) rotation angle.
See : K Ferrière, J L West, T R Jaffe, The correct sense of Faraday rotation, MNRAS.
2.
From Salome Mtchedlidze. Magnetic field strength in cosmological simulations, see :
https://arxiv.org/abs/2109.13520
3.
From Dr. Prantika Bhowmik.
4.
From Prof Maarit Kapyla. Solar models showing the measured turbulent transport coefficients (in this case alpha_phi_phi) with the quasi-kinematic test-field method in the meridional planes. On the surface we show the velocity field, and in the background there is a SDO image of the Sun.
See : K ̈apyl ̈a, M.,J.,Viviani, M., Prabhu, A., Warnecke, J., Duarte, L., Pekkil ̈a, J., Rheinhardt, M.: ’Hunting down the cause of solar magnetism’, in ”High Performance Computing Science and Engineering, Garching/Munich, 2020”, p. 26–28, editors: P. Bastina, D. Kranzmu ̈ller, H. Br ̈euchle, M. Brehm. ISBN: 978-3-9816675-4-7, arXiv:2102.03168
5.
From Prof Pallavi Bhat. The y-component of the magnetic field from a dynamo simulation with helical forcing and shear. See: https://arxiv.org/abs/1905.08278
6.
From Dr. Paola Dominguez Fernandez.
7.
From Dr. Anna Guseva. Components of the magnetic field from an MRI unstable system.
8.
From Prof. Yuri Fujii. An artistic view of satellite formation.
9.
From Prof Katia Ferriere.
The left panel shows a small sky area observed by Herschel, with a distinct interstellar dust filament in the center and the shape of magnetic field lines in the background.
The H2 column density was derived by combining Herschel data at several wavelengths and adopting a dust-to-gas conversion factor, while the shape of field lines was inferred from Planck polarization data at 353 GHz.
The right panel shows the filament that we extracted from the H2 map, using a new reconstruction method.
The purpose of our work is to study the relative orientation between dense interstellar filaments and the local magnetic field.
10.
From Sriyasriti Acharya. This figure shows the synchrotron intensity maps of the plasma column for different viewing angles of the observer and demonstrates the effect of relativistic Doppler boosting.
11.
From Dr. Prakriti Pal Choudhuri.
Simulation of central 40-50kpc of a galaxy-cluster. Shown velocity field with streamlines.
12.
From Prof Pallavi Bhat. Evolution of current density from a decaying MHD turbulence simulation. It can be seen that current sheets are growing over a period of time pointing towards the possibility of magnetic reconnection that can occur at these sites.
See : Pallavi Bhat, Muni Zhou, Nuno F Loureiro, Inverse energy transfer in decaying, three-dimensional, non-helical magnetic turbulence due to magnetic reconnection, Monthly Notices of the Royal Astronomical Society, Volume 501, Issue 2, February 2021, Pages 3074–3087, https://doi.org/10.1093/mnras/staa3849
- Log in to post comments