RHESSI - Concept to Fruition

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To study the core nonthermal physics of the flare, hard X-ray [http://en.wikipedia.org/wiki/Bremsstrahlung bremsstrahlung] and radio [http://en.wikipedia.org/wiki/Synchrotron_radiation gyrosynchrotron radiation] have proven to be the most interesting, although there are many other direct and indirect manifestations.
To study the core nonthermal physics of the flare, hard X-ray [http://en.wikipedia.org/wiki/Bremsstrahlung bremsstrahlung] and radio [http://en.wikipedia.org/wiki/Synchrotron_radiation gyrosynchrotron radiation] have proven to be the most interesting, although there are many other direct and indirect manifestations.
RHESSI has provided the best view to date of the hard X-ray bremsstrahlung, while at the same timing doing remarkably new things such as gamma-ray imaging and spectroscopy.
RHESSI has provided the best view to date of the hard X-ray bremsstrahlung, while at the same timing doing remarkably new things such as gamma-ray imaging and spectroscopy.
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These Nuggets (both the [http://sprg.ssl.berkeley.edu/~tohban/nuggets/ old series] and our current [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI_Science_Nuggets Wiki series] provide many glimpses into these discoveries.
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These Nuggets (both the [http://sprg.ssl.berkeley.edu/~tohban/nuggets/ old series] and our current [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/RHESSI_Science_Nuggets Wiki series]) provide many glimpses into these discoveries.
Where does RHESSI fit in the history of hard X-ray solar science?
Where does RHESSI fit in the history of hard X-ray solar science?
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There were three previous hard X-ray imagers: a [rotating modulation collimator] on the [Hinotori] spacecraft; a multi-grid collimator on the [Solar Maximum Mission], an array of fixed bigrid collimators on [Yohkoh], and now our multiple rotating collimators on RHESSI.
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There were three previous hard X-ray imagers: a [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=8 rotating modulation collimator] on the [http://www.daviddarling.info/encyclopedia/H/Hinotori.html Hinotori] spacecraft; a multi-grid collimator on the [http://www.daviddarling.info/encyclopedia/S/SMM.html Solar Maximum Mission], an array of fixed bigrid collimators on [http://www.daviddarling.info/encyclopedia/Y/Yohkoh.html Yohkoh], and now our multiple rotating collimators on RHESSI.
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These three predecessor instruments were all quite distinct, even though they all relied upon modulation imaging - only now are we beginning to get the technology needed for [http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=62 hard X-ray imaging with mirrors].
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RHESSI provided tremendous improvements over its predecessors in most observing properties.
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== RHESSI's proposal history ==
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To get RHESSI into orbit (February 2002, in time to see the previous solar maximum and possibly the [sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Cycle_24_-_don%27t_panic_yet%21 next one] as well) required a great deal of preparation.
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Two U.S. laboratories needed to combine their efforts (the [http://www.ssl.berkeley.edu/ Space Sciences Lab] at Berkeley, and NASA's [http://hesperia.gsfc.nasa.gov/hessi/ Goddard Space Flight Center]) with the aid of major Swiss contributions (the [http://www.psi.ch/index_e.shtml Paul Scherrer Institute] and [http://www.ethz.ch/ ETH].
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== RHESSI's proposal history ==
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== The key people ==
== The key people ==
== Conclusions ==
== Conclusions ==

Revision as of 21:01, 27 April 2009


Nugget
Number: 100
1st Author: Hugh Hudson
2nd Author:
Published: 27 April 2009
Next Nugget: Austrian microflares
Previous Nugget: Cycle 24 - don't panic yet!
List all



Contents

Introduction

Our RHESSI (the Reuven Ramaty High-Energy Solar Spectroscopic Imager) has a rich history, and we take the opportunity to devote RHESSI Science Nugget number 100 to a review of how RHESSI came to be. The Nuggets are roughly biweekly, and the first RHESSI Science Nugget was put on line on 21 March 2005 - a few years after RHESSI's launch date, and three years after the discoveries began. The Nuggets are an informal channel for publicizing RHESSI (and solar) discoveries, and the dozens of volunteer authors work towards making them readable by all. This seems to work - the previous Nugget 99 has had 1,301 Web accesses in its first two weeks. This level of citation of a scientific paper might attract the attention of the Nobel Prize committee!

Hard X-ray imaging

At their core, solar flares are highly nonthermal in nature. That is, they involve highly intense energy release in a manner characterized by short time scales (below one sec) and small spatial scales (below a few arc sec); on larger scales they are also involved in the gigantic and beautiful eruptions termed CMEs. To study the core nonthermal physics of the flare, hard X-ray bremsstrahlung and radio gyrosynchrotron radiation have proven to be the most interesting, although there are many other direct and indirect manifestations. RHESSI has provided the best view to date of the hard X-ray bremsstrahlung, while at the same timing doing remarkably new things such as gamma-ray imaging and spectroscopy. These Nuggets (both the old series and our current Wiki series) provide many glimpses into these discoveries.

Where does RHESSI fit in the history of hard X-ray solar science? There were three previous hard X-ray imagers: a rotating modulation collimator on the Hinotori spacecraft; a multi-grid collimator on the Solar Maximum Mission, an array of fixed bigrid collimators on Yohkoh, and now our multiple rotating collimators on RHESSI. These three predecessor instruments were all quite distinct, even though they all relied upon modulation imaging - only now are we beginning to get the technology needed for hard X-ray imaging with mirrors. RHESSI provided tremendous improvements over its predecessors in most observing properties.

RHESSI's proposal history

To get RHESSI into orbit (February 2002, in time to see the previous solar maximum and possibly the [sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Cycle_24_-_don%27t_panic_yet%21 next one] as well) required a great deal of preparation. Two U.S. laboratories needed to combine their efforts (the Space Sciences Lab at Berkeley, and NASA's Goddard Space Flight Center) with the aid of major Swiss contributions (the Paul Scherrer Institute and ETH.

The key people

Conclusions

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