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Instrumentation and Analysis Tools for Studying Solar Spicules in the Sun's Upper Chromosphere /

Record Type:	Electronic resources : Monograph/item
Title/Author:	Instrumentation and Analysis Tools for Studying Solar Spicules in the Sun's Upper Chromosphere // Vicki Herde.
Author:	Herde, Vicki,
Description:	1 electronic resource (122 pages)
Notes:	Source: Dissertations Abstracts International, Volume: 86-06, Section: B.
Contained By:	Dissertations Abstracts International86-06B.
Subject:	Astrophysics. -
Online resource:	https://pqdd.sinica.edu.tw/twdaoapp/servlet/advanced?query=31636676
ISBN:	9798346877257

Instrumentation and Analysis Tools for Studying Solar Spicules in the Sun's Upper Chromosphere /
Herde, Vicki,

Instrumentation and Analysis Tools for Studying Solar Spicules in the Sun's Upper Chromosphere /Vicki Herde. - 1 electronic resource (122 pages)

Source: Dissertations Abstracts International, Volume: 86-06, Section: B.

The Sun's chromosphere is a critical region to understand when considering energy and mass deposition into the transition region and corona, but many of the faster events such as solar spicules which transport a portion of this mass and energy are still difficult to identify and model. Solar Spicules are small, spike-like events in the solar chromosphere that have the potential to transfer energy and mass to the transition region, but whose energetic origins are still being researched. Chromospheric spicule activity on-disk can be identified by observing temporary excursions in the red and blue wings of chromospheric emission lines. Researchers have demonstrated this in Hydrogen Alpha (Hα, 6563 ˚A), Ca ii (8542 ˚A, k 3934 ˚A), Mg ii (h 2803 ˚A, k 2796 ˚A), and Si iv (1394 ˚A, 1405 ˚A) spectral observations, with the vast majority of identification efforts focused on lower chromospheric observations of Hα and Ca ii. Because any spicules which deposit mass and energy into the transition region must necessarily pass through the upper chromosphere, Mg ii and Hydrogen Lyman Alpha (Lyα 1216 ˚A) observations in enough quantity to perform proper statistics will be critical to fully characterizing spicules' impact on mass and energy transfer in the Sun. In this thesis, two new methods for observing and identifying upper-chromospheric spicules in large quantities to further our understanding of these events are presented. The first is an algorithm for automatically detecting spicules in Mg ii spectral data to help allow statistical studies on spicules in the upper chromosphere to be as thorough as those of the lower chromosphere. The second is the design and development of a novel integral field spectrograph to observe upper chromosphere (Lyα) and transition region (Si iii, O v) emission lines in order to observe spicules and their evolution over multiple unstudied heights in the solar atmosphere. This research explores the hypothesis that Mg II spectral observations can be used to provide a large number of on-disk upper-chromospheric spicule identifications for the purpose of statistical studies, and a new design of integral field spectrograph can meet requirements to observe solar spicules in Lyα, Si iii, and O v wavelengths for further study.The following questions serve as a guide to address the above hypothesis and a roadmap for the structure of this dissertation.(1) How can spicule signatures be quantified in Mg ii spectral observations on the solar disk, and can these signatures be autonomously or algorithmically identified in large or multiple datasets?(2) How do these Mg II spicule identifications compare to other studies with regard to quantity, location, and duration, particularly those which observe different stages of spicule evolution?(3) What is the relationship between photospheric magnetic field strength and spicule occurrence in middle- and upper-chromospheric observations?(4) What is needed to design and build a new type of integral field spectrograph which meets the requirements to see spicules in ultraviolet spectral observations?Answering these questions provides tools for researchers to better understand the chromospheric-transition region connection. The ability to identify upper chromospheric spicules in large quantities will allow researchers to more thoroughly compare lower chromospheric activity to that of the region above, while the ability to observe spicules spatially and spectrally in upper chromospheric and transition region wavelengths will unlock the final observation connections of fast-changing events between the lower chromosphere and the transition region. With this, the physical nature of spicules and their role in energy deposition and mass transfer in the solar atmosphere will be more well understood.

English

ISBN: 9798346877257Subjects--Topical Terms:

535904
Astrophysics.
Subjects--Index Terms:

Chromosphere

Instrumentation and Analysis Tools for Studying Solar Spicules in the Sun's Upper Chromosphere /
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520 $a The Sun's chromosphere is a critical region to understand when considering energy and mass deposition into the transition region and corona, but many of the faster events such as solar spicules which transport a portion of this mass and energy are still difficult to identify and model. Solar Spicules are small, spike-like events in the solar chromosphere that have the potential to transfer energy and mass to the transition region, but whose energetic origins are still being researched. Chromospheric spicule activity on-disk can be identified by observing temporary excursions in the red and blue wings of chromospheric emission lines. Researchers have demonstrated this in Hydrogen Alpha (Hα, 6563 ˚A), Ca ii (8542 ˚A, k 3934 ˚A), Mg ii (h 2803 ˚A, k 2796 ˚A), and Si iv (1394 ˚A, 1405 ˚A) spectral observations, with the vast majority of identification efforts focused on lower chromospheric observations of Hα and Ca ii. Because any spicules which deposit mass and energy into the transition region must necessarily pass through the upper chromosphere, Mg ii and Hydrogen Lyman Alpha (Lyα 1216 ˚A) observations in enough quantity to perform proper statistics will be critical to fully characterizing spicules' impact on mass and energy transfer in the Sun. In this thesis, two new methods for observing and identifying upper-chromospheric spicules in large quantities to further our understanding of these events are presented. The first is an algorithm for automatically detecting spicules in Mg ii spectral data to help allow statistical studies on spicules in the upper chromosphere to be as thorough as those of the lower chromosphere. The second is the design and development of a novel integral field spectrograph to observe upper chromosphere (Lyα) and transition region (Si iii, O v) emission lines in order to observe spicules and their evolution over multiple unstudied heights in the solar atmosphere. This research explores the hypothesis that Mg II spectral observations can be used to provide a large number of on-disk upper-chromospheric spicule identifications for the purpose of statistical studies, and a new design of integral field spectrograph can meet requirements to observe solar spicules in Lyα, Si iii, and O v wavelengths for further study.The following questions serve as a guide to address the above hypothesis and a roadmap for the structure of this dissertation.(1) How can spicule signatures be quantified in Mg ii spectral observations on the solar disk, and can these signatures be autonomously or algorithmically identified in large or multiple datasets?(2) How do these Mg II spicule identifications compare to other studies with regard to quantity, location, and duration, particularly those which observe different stages of spicule evolution?(3) What is the relationship between photospheric magnetic field strength and spicule occurrence in middle- and upper-chromospheric observations?(4) What is needed to design and build a new type of integral field spectrograph which meets the requirements to see spicules in ultraviolet spectral observations?Answering these questions provides tools for researchers to better understand the chromospheric-transition region connection. The ability to identify upper chromospheric spicules in large quantities will allow researchers to more thoroughly compare lower chromospheric activity to that of the region above, while the ability to observe spicules spatially and spectrally in upper chromospheric and transition region wavelengths will unlock the final observation connections of fast-changing events between the lower chromosphere and the transition region. With this, the physical nature of spicules and their role in energy deposition and mass transfer in the solar atmosphere will be more well understood.
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653 $a Coronal heating problem
653 $a Instrumentation
653 $a Solar
653 $a Spectrograph
653 $a Spicules
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