Observations of loops and prominences

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National Aeronautics and Space Administration, National Technical Information Service, distributor , [Washington, DC, Springfield, Va
StatementKeith T. Strong and the Yokoh team.
Series[NASA contractor report] -- 195942., NASA contractor report -- NASA CR-195942.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
FormatMicroform
Pagination1 v.
ID Numbers
Open LibraryOL14667862M

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In XBP flares, for example, velocities of over km/s are common. Active-region loops seem to be in constant motion, moving slowly outward, carrying plasma with them. During flares, loops often produce localized brightenings at the base and later at the apex of the loop. Quiescent filaments and prominences have been observed by: 1.

We review recent observations by the Yohkoh-SXT in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences.

These new results point to problems that SoHO will be able to address. With a unique combination of rapid-cadence digital imaging (≥32 s full-disk and ≥2 s partial-frame images), high spatial resolution (≥ arcsec pixels), high Cited by: 5.

We review recent observations by the Yohkoh-SXT (Soft X-ray Telescope) in collaboration with other spacecraft and ground-based observatories of coronal loops and prominences. These new results point to problems that SoHO will be able to address.

Observations of loops and prominences book With a unique combination of rapid-cadence digital imaging (greater than or equal to 32 s full-disk and greater than or equal to 2 s Cited by: 1. Abstract. We had a lively session on the subjects of prominences and loops stimulated by excellent reviews earlier in the day on Yohkoh observations by Keith Strong, the theory of loop flows by Spiro Antiochos and how SOHO can observe loop flows by Ester : E.

Priest. The comparison of the RATAN data with optical observations of coronal loops in the green line and with the Very Large Array maps at 21 cm has shown that the loops represent only a small part of coronal matter, although their role may be of great importance in the physics of the solar corona.

Topics discussed ranged from solar flux ropes, such as photospheric flux tubes, coronal loops and prominences, to flux ropes in the solar wind, in planetary ionospheres, at the Earth's magnetopause, in the geomagnetic tail and deep in the Earth's magnetosphere. Observations are considered, taking into account a morphology and physical properties.

Loop prominences as a reconnection process are discussed along with magnetic field dynamics, giving attention to the response of the plasma to magnetic field line motion, the shock wave, the filament, and relaxation and reconnection.

We briefly review the multiwavelength observations of solar prominences and filaments ranging from the infrared up to soft X-rays. We give several examples of current observations and mention those specific to the total solar eclipses.

Our particular focus is on the ultraviolet (UV) and extreme-UV images taken in various lines of different species. These loops of plasma are solar prominences, and they can measure many times larger than Earth’s diameter.

Prominences push out into the Sun’s thin, extremely hot atmosphere, called the corona. During the last few years, high quality space-based observations have shown evidence for waves and oscillations in a wide variety of solar structures, such as coronal loops, polar plumes and prominences.

In this review, observations of propagating, slow waves and standing, fast modes in the solar corona are summarized and examples are given of.

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Observation of Loop-Type Prominences in Projection against the Disk at the Time of Certain Solar Flares. For some time to come, this book should be the main source for research in prominences.

It surveys the results of the past years, including the "Hvar Reference Atmosphere", which was developed by a panel as a model for quiescent prominences. Radial velocity observations of prominences (Arkiv för astronomi) [Liszka, Ludwik] on *FREE* shipping on qualifying offers.

Radial velocity observations of prominences (Arkiv för astronomi)Author: Ludwik Liszka. Features, such as flare loops, spicules, and surges acquired separate identities and no longer needed to be classified as prominences. Observations with increased spatial resolution allowed the identity of fine thread-like structure within the basic spine and barb structure of filaments.

These observations provide important tests for models of dynamics in prominences and cool (~ K) loops, which will ultimately lead to a better understanding of the mechanism(s) leading to energy. Some, the quiescent prominences, are graceful loops of plasma (ionized gas) that can remain nearly stable for many hours or even days.

The relatively rare eruptive prominences appear to send matter upward into the corona at high speeds, and the most active surge prominences may move as fast as kilometers per second (almost 3 million miles. Estimation of the line of sight amplitude of the magnetic field on threads of an active region prominence.- High resolution observations of motions and structure of prominence threads.- Observational aspects of a prominence from HeI data analysis.- Some observations of the coronal environment of prominences Recent observations and models of solar prominences are reviewed.

The observations suggest that prominences are located in or below magnetic flux ropes that lie horizontally above the PIL. Samples from 10 Years of EIT Observations () Movie available in the following formats and sizes: MPEG (35M), MPEG (11M), QT (60M), QT (60M), QT (M) Highlights from 10 Years of SOHO Observations.

Movie available in the following formats and sizes: MPEG (11M), QT (11M), QT (M) Filaments and prominences. nd The 2 SORO Workshop on "Mass Supply and Flows in the Solar Corona" was held in Marciana Mariana on the island of Elba, Italy, in the week September 27 to October 1,as part of a series of workshops planned by the Solar Corona and Particles Working.

This time-lapse film shows active prominences of a few hours' duration. “Loop” prominences like this one, which seems to rise and fall back to the surface, are the aftermath of solar flares. Prominences are transparent in normal light and have to be viewed through special instruments that can detect the spectroscopic emission lines of hydrogen.

proc natl acad sci u s a. jul;47(7) observation of loop-type prominences in projection against the disk at the time of certain solar flares. A comprehensive study on the loop prominence will provide further data for a deeper investigation of the structure, the field distribution and the law of motion in the active regions and flares.

In the past, simultaneous monochromatic and spectral observations of loop prominences were few.

Details Observations of loops and prominences EPUB

A prominence is a large, bright, gaseous feature extending outward from the Sun's surface, often in a loop ences are anchored to the Sun's surface in the photosphere, and extend outwards into the solar the corona consists of extremely hot ionized gases, known as plasma, which do not emit much visible light, prominences contain much cooler plasma, similar in composition.

2 days ago  The best stills of magnetic loops and prominences MPEG (M), MPEG (M), QT (M), QT (M) Several active regions and loops, EIT (Nov.). We had a lively session on the subjects of prominences and loops stimulated by excellent reviews earlier in the day on Yohkoh observations by Keith Strong, the theory of loop flows by Spiro.

Prominences are amazing objects of great beauty whose formation, basic structure and eruption represent one of the basic unsolved problems in Solar Physics.

It is now 14 years since the last book on prominences appeared (Tandberg-Hanssen, ), during which time much progress in our knowledge of the physics of prominences has been made, and so the time is ripe for a new text book which it is. On the Support of Loop Prominences.

Description Observations of loops and prominences EPUB

Article. Dec ; Starting with the observation that most prominences are of the inverse topology, a recent model is extended to show that this topology. At the XV. General Assembly of the International Astronomical Union in SydneyCommission 10 for Solar Activity requested the incoming Organising Committee to establish a small group to recommend a standard nomenclature for solar features and to prepare an illustrated text which would clear the jungle of terms for the benefit of solar physicists as well as of theoreticians and.

Foukal studied these cool loops in detail from the observations taken with the EUV spectrometer on Skylab in Otherwise, when the plasma temperature of these loops becomes coronal (above 1 MK), these features appear more stable and evolve on longer times.

See the flash spectrum of the solar chromosphere (Eclipse of March 7, ). Coronal Loops. Coronal loops are found around sunspots and in active regions. These structures are associated with the closed magnetic field lines that connect magnetic regions on the solar surface.

Many coronal loops last for days or weeks but most change quite rapidly (10 Mb Quicktime movie from TRACE observations). Large impressive loop-like structures on the edge of the solar disk sometimes stand out brightly against the dark background of space.

Though these structures, called "prominences", appear to be very bright and hot, they are actually hundreds of times cooler and denser than the surrounding gases in the Sun's corona or outermost atmosphere.