dc.contributor.author |
Panini, S. S |
|
dc.contributor.author |
Narendranath, S |
|
dc.contributor.author |
Sreekumar, P |
|
dc.contributor.author |
Sankarasubramanian, K |
|
dc.date.accessioned |
2022-08-03T05:06:01Z |
|
dc.date.available |
2022-08-03T05:06:01Z |
|
dc.date.issued |
2021-07 |
|
dc.identifier.citation |
Frontiers in Astronomy and Space Sciences, Vol. 8, 647828 |
en_US |
dc.identifier.issn |
2296-987X |
|
dc.identifier.uri |
http://hdl.handle.net/2248/7985 |
|
dc.description |
Open Access |
en_US |
dc.description |
This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms. |
|
dc.description.abstract |
Soft X-ray spectroscopy of the Sun is an important tool to understand the coronal
dynamics and composition. The solar coronal X-ray spectrum below 1 keV is the least
explored with high-resolution spectroscopy. Recent observations with Hinode XRT using
coarse spectroscopy along with high-resolution imaging have shown that abundances in
the coronae have variability associated with structures on the Sun. Disk averaged
abundances with better spectral resolution spectrometers show time variability
associated with flares. Both spatial and temporal variabilities seem to be related to
changes in the magnetic field topology. Understanding such short term variabilities is
necessary to model the underlying dynamics and mixing of material between different
layers of the Sun. A Sensitive high-resolution spectrometer that covers the range in plasma
temperatures and emission line complexes would uniquely reveal the entire evolution of
flares. We are investigating a design of a multi-layer mirror-based X-ray spectrograph in the
spectral range from 0.5 to 7 keV. The instrument operates in four asynchronous spectral
channels operating one at a time. The multi-layer mirror placed at the focus of a Wolter type
I telescope reflects a narrow band X-rays to the CCD which is placed at Nasmyth defocus.
Converging X-rays from the front end optics helps to increase the spectral range of each
channel while preserving the spectral resolution. This design is estimated to achieve a
spectral resolution of 20 eV in the spectral range of 0.5–7 keV. With such high spectral
resolution, we can resolve individual spectral features e.g., 6.7 keV Fe complex which can
be used to diagnose high-temperature transient plasma during flares. The instrument
design estimated performance and the science capabilities of this instrument will be
discussed in detail in the paper. |
en_US |
dc.language.iso |
en |
en_US |
dc.publisher |
Frontiers Media S.A |
en_US |
dc.relation.uri |
https://doi.org/10.3389/fspas.2021.647828 |
|
dc.rights |
© 2022 Frontiers Media S.A |
|
dc.subject |
Solar corona |
en_US |
dc.subject |
X-ray spectroscopy |
en_US |
dc.subject |
X-ray telescope |
en_US |
dc.subject |
Multilayer mirror |
en_US |
dc.subject |
X-rays |
en_US |
dc.title |
Multilayer Mirror Based High-Resolution Solar Soft X-Ray Spectrometer |
en_US |
dc.type |
Article |
en_US |