Calibration of spectropolarimetry channel of visible emission line coronagraph onboard Aditya-L1

IF 2.7 3区物理与天体物理 Q2 ASTRONOMY & ASTROPHYSICS

Experimental Astronomy Pub Date : 2024-09-13 DOI:10.1007/s10686-024-09954-8

Venkata Suresh Narra, K. Sasikumar Raja, Raghavendra Prasad B, Jagdev Singh, Shalabh Mishra, Sanal Krishnan V U, Bhavana Hegde S, Utkarsha D., Natarajan V, Pawan Kumar S, Muthu Priyal V, Savarimuthu P, Priya Gavshinde, Umesh Kamath P

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Abstract

The magnetic field strength and its topology play an important role in understanding the formation, evolution, and dynamics of the solar corona. Also, it plays a significant role in addressing long-standing mysteries such as coronal heating problem, origin and propagation of coronal mass ejections, drivers of space weather, origin and acceleration of solar wind, and so on. Despite having photospheric magnetograms for decades, we do not have reliable observations of coronal magnetic field strengths today. To measure the coronal magnetic field precisely, the spectropolarimetry channel of the Visible Emission Line Coronagraph (VELC) on board the Aditya-L1 mission is designed. Using the observations of coronal emission line Fe XIII [10747Å ], it is possible to generate full Stokes maps (I, Q, U, and V) that help in estimating the Line-of-Sight (LOS) magnetic field strength and to derive the magnetic field topology maps of solar corona in the Field of View (FOV) (1.05 – 1.5 R\(_{\odot }\)). In this article, we summarize the instrumental details of the spectropolarimetry channel and detailed calibration procedures adopted to derive the modulation and demodulation matrices. Furthermore, we have applied the derived demodulation matrices to the observed data in the laboratory and studied their performance.

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校准 Aditya-L1 上可见发射线日冕仪的摄谱仪通道

磁场强度及其拓扑结构对了解日冕的形成、演变和动力学起着重要作用。此外，它在解决日冕加热问题、日冕物质抛射的起源和传播、空间天气的驱动因素、太阳风的起源和加速等长期未解之谜方面也发挥着重要作用。尽管几十年来我们一直拥有光球层磁图，但今天我们还没有可靠的日冕磁场强度观测数据。为了精确测量日冕磁场，设计了 Aditya-L1 飞行任务上的可见发射线日冕仪（VELC）的分光测极仪通道。利用对日冕发射线 Fe XIII [10747Å ]的观测，可以生成完整的斯托克斯图（I、Q、U 和 V），这有助于估算视线（LOS）磁场强度，并得出日冕在视场（FOV）（1.05 - 1.5 R\(_{\odot }\) ）内的磁场拓扑图。在这篇文章中，我们总结了分光测极仪信道的仪器细节，以及为得出调制和解调矩阵而采用的详细校准程序。此外，我们还将得出的解调矩阵应用于实验室观测数据，并研究了它们的性能。

本文章由计算机程序翻译，如有差异，请以英文原文为准。

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来源期刊

Experimental Astronomy 地学天文-天文与天体物理

CiteScore

5.30

自引率

3.30%

发文量

审稿时长

6-12 weeks

期刊介绍： Many new instruments for observing astronomical objects at a variety of wavelengths have been and are continually being developed. Furthermore, a vast amount of effort is being put into the development of new techniques for data analysis in order to cope with great streams of data collected by these instruments. Experimental Astronomy acts as a medium for the publication of papers of contemporary scientific interest on astrophysical instrumentation and methods necessary for the conduct of astronomy at all wavelength fields. Experimental Astronomy publishes full-length articles, research letters and reviews on developments in detection techniques, instruments, and data analysis and image processing techniques. Occasional special issues are published, giving an in-depth presentation of the instrumentation and/or analysis connected with specific projects, such as satellite experiments or ground-based telescopes, or of specialized techniques.

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