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Coronal Temperature Diagnostics Derived From
CORONAL TEMPERATURE DIAGNOSTICS DERIVED FROM MULTILAYER OBSERVATIONS WITH THE MULTI-SPECTRAL SOLAR TELESCOPE ARRAY A DISSERTATION SUBMITTED TO THE DEPARTMENT OF PHYSICS AND THE COMMITTEE ON GRADUATE STUDIES OF STANFORD UNIVERSITY IN PARTIAL FULFILLMENT OF THE REQUIREMENTS FOR THE DEGREE OF DOCTOR OF PHILOSOPHY Paul Boerner July 2004 © Copyright by Paul Boerner 2004 All Rights Reserved ii I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. _____________________________________________ Philip Scherrer Principal Adviser I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. _____________________________________________ Sarah Church I certify that I have read this dissertation and that, in my opinion, it is fully adequate in scope and quality as a dissertation for the degree of Doctor of Philosophy. _____________________________________________ Vahé Petrosian Approved for the University Committee on Graduate Studies: _____________________________________________ iii iv ABSTRACT In recent years, satellite-based extreme ultraviolet multilayer telescopes observing the solar corona have provided some of the most beautiful and fascinating images ever seen. However, our ability to extract quantitative information about the thermodynamic state of the solar atmosphere from these images has been limited by their broad temperature response, uncertain calibration status, and the limited number of bandpasses available. In this dissertation, I present a unique dataset and novel analysis techniques designed to provide rigorous constraints on conditions in the corona with the high spatial and temporal resolution of multilayer images. -
Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations
Space Sci Rev (2007) 133: 103–179 DOI 10.1007/s11214-007-9285-0 Observations of the Sun at Vacuum-Ultraviolet Wavelengths from Space. Part II: Results and Interpretations Klaus Wilhelm · Eckart Marsch · Bhola N. Dwivedi · Uri Feldman Received: 22 February 2007 / Accepted: 9 October 2007 / Published online: 9 January 2008 © Springer Science+Business Media B.V. 2008 Abstract In Part I of this review, the concepts of solar vacuum-ultraviolet (VUV) obser- vations were outlined together with a discussion of the space instrumentation used for the investigations. A section on spectroradiometry provided some quantitative results on the solar VUV radiation without considering any details of the solar phenomena leading to the radiation. Here, in Part II, we present solar VUV observations over the last decades and their interpretations in terms of the plasma processes and the parameters of the solar atmosphere, with emphasis on the spatial and thermal structures of the chromosphere, transition region and corona of the quiet Sun. In addition, observations of active regions, solar flares and prominences are included as well as of small-scale events. Special sections are devoted to the elemental composition of the solar atmosphere and theoretical considerations on the heating of the corona and the generation of the solar wind. Keywords Solar VUV—observations and interpretations · Solar atmosphere · Solar plasma processes and parameters Abbreviations ACE Advanced Composition Explorer BCS Bragg Crystal Spectrometer K. Wilhelm () · E. Marsch · B.N. Dwivedi Max-Planck-Institut für Sonnensystemforschung (MPS), Max-Planck-Str. 2, 37191 Katlenburg-Lindau, Germany e-mail: [email protected] B.N. Dwivedi Department of Applied Physics, Institute of Technology, Banaras Hindu University, Varanasi 221005, India U. -
![Arxiv:2102.02943V2 [Astro-Ph.SR] 17 Mar 2021 Is Widely Used in Solar Physics for Modeling Emission Lines](https://docslib.b-cdn.net/cover/6902/arxiv-2102-02943v2-astro-ph-sr-17-mar-2021-is-widely-used-in-solar-physics-for-modeling-emission-lines-8546902.webp)
Arxiv:2102.02943V2 [Astro-Ph.SR] 17 Mar 2021 Is Widely Used in Solar Physics for Modeling Emission Lines
Future Prospects for Solar EUV and Soft X-ray Spectroscopy Missions Peter R. Young 1;2;∗ 1NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA 2Northumbria University, Newcastle upon Tyne, NE1 8ST, UK Correspondence*: NASA Goddard Space Flight Center, Code 671, Greenbelt, MD 20771, USA [email protected] ABSTRACT Future prospects for solar spectroscopy missions operating in the extreme ultraviolet (EUV) and soft X-ray (SXR) wavelength ranges, 1.2–1600 Å, are discussed. NASA is the major funder of Solar Physics missions, and brief summaries of the opportunities for mission development under NASA are given. Upcoming major solar missions from other nations are also described. The methods of observing the Sun in the two wavelength ranges are summarized with a discussion of spectrometer types, imaging techniques and detector options. The major spectral features in the EUV and SXR regions are identified, and then the upcoming instruments and concepts are summarized. The instruments range from large spectrometers on dedicated missions, to tiny, low-cost CubeSats launched through rideshare opportunities. Keywords: keyword, keyword, keyword, keyword, keyword, keyword, keyword, keyword 1 INTRODUCTION This paper discusses prospects for future extreme ultraviolet (EUV) and soft X-ray (SXR) spectroscopic missions observing the Sun. It is based on presentations given by the author at the 2018 American Geophysical Union meeting and the 2019 RHESSI Workshop.1 The EUV and SXR contain a huge number of narrow emission lines from many different elements and ion species formed in all layers of the solar atmosphere, and spectroscopy plays a critical role in understanding the physics occurring there. -
Coronal Loops: Observations and Modeling of Confined Plasma
Living Rev. Solar Phys., 11, (2014), 4 ,)6).' 2%6)%73 http://www.livingreviews.org/lrsp-2014-4 doi:10.12942/lrsp-2014-4 INSOLARPHYSICS Coronal Loops: Observations and Modeling of Confined Plasma Fabio Reale Dipartimento di Fisica & Chimica, Universit`adi Palermo, Piazza Parlamento 1, 90134 Palermo, Italy email: [email protected] http://www.astropa.unipa.it/~reale/ Accepted: 23 June 2014 Published: 29 July 2014 (Update of lrsp-2010-5) Abstract Coronal loops are the building blocks of the X-ray bright solar corona. They owe their brightness to the dense confined plasma, and this review focuses on loops mostly as structures confining plasma. After a brief historical overview, the review is divided into two separatebut not independent parts: the first illustrates the observational framework, the second reviews the theoretical knowledge. Quiescent loops and their confined plasma are considered and, therefore, topics such as loop oscillations and flaring loops (except for non-solar ones, which provide information on stellar loops) are not specifically addressed here. The observational section discusses the classification, populations, and the morphology of coronal loops, its relationship with the magnetic field, and the loop stranded structure. The section continues with the thermal properties and diagnostics of the loop plasma, according to the classification into hot, warm, and cool loops. Then, temporal analyses of loops and the observations of plasma dynamics, hot and cool flows, and waves are illustrated. In the modeling section, some basics of loop physics are provided, supplying fundamental scaling laws and timescales, a useful tool for consultation. The concept of loop modeling is introduced and models are divided into those treating loops as monolithic and static, and those resolving loops into thin and dynamic strands. -
Coronal Loops: Observations and Modeling of Confined Plasma
Coronal Loops: Observations and Modeling of Confined Plasma Fabio Reale Dipartimento di Scienze Fisiche & Astronomiche, Universit`adi Palermo, Sezione di Astronomia, Piazza Parlamento 1, 90134 Palermo, Italy email: [email protected] http://www.astropa.unipa.it/~reale/ Abstract Coronal loops are the building blocks of the X-ray bright solar corona. They owe their brightness to the dense confined plasma, and this review focuses on loops mostly as structures confining plasma. After a brief historical overview, the review is divided into two separate but not independent sections: the first illustrates the observational framework, the second reviews the theoretical knowledge. Quiescent loops and their confined plasma are considered, and therefore topics such as loop oscillations and flaring loops (except for non-solar ones which provide information on stellar loops) are not specifically addressed here. The observational section discusses loop classification and populations, and then describes the morphology of coronal loops, its relationship with the magnetic field, and the concept of loops as multi- stranded structures. The following part of this section is devoted to the characteristics of the loop plasma, and of its thermal structure in particular, according to the classification into hot, warm and cool loops. Then, temporal analyses of loops and the observations of plasma dynamics and flows are illustrated. In the modeling section starts some basics of loop physics are provided, supplying some fundamental scaling laws and timescales, a useful tool for consultation. The concept of loop modeling is introduced, and models are distinguished between those treating loops as monolithic and static, and those resolving loops into thin and dynamic strands.