Glasgow Callisto optimistic: first light comes in focus

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{{Infobox Nugget
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|name = Nugget
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|title = Glasgow Callisto optimistic: first light comes in focus
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|number = 187
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|first_author = Heather Ratcliffe
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|second_author =  Eduard Kontar
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|publish_date = 29 October 2012
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|next_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/%22Impulse_Response_Flares%22_and_Gamma_Rays Impulse Response]
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|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Photospheric_Temperature_Gradient Photospheric Temperature]
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}}
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== Introduction ==
== Introduction ==
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Hard X-Ray (HXR) bursts and Solar Type III radio bursts are some of the commonest solar emissions caused by energetic electrons. In the well-known solar flare cartoon, electron acceleration produces beams propagating both downwards and upwards along magnetic field lines. The downwards going beam propagates along closed loops and produces HXR emission by collisional bremsstrahlung. The signature of the upwards going beam is a Type III radio burst, which occurs at the local plasma frequency or its harmonics. As the beam propagates away from the sun along open magnetic field lines, it encounters plasma of rapidly decreasing density, so emission occurs at rapidly decreasing frequency, giving Type IIIs a characteristic "hockey stick" shape.  
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Hard X-Ray (HXR) bursts and solar
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[http://solarphysics.livingreviews.org/open?pubNo=lrsp-2006-2&page=articlesu11.html Type III radio bursts] are some of the commonest solar emissions caused by energetic electrons. In a well-known  
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[http://solarmuri.ssl.berkeley.edu/~hhudson/cartoons/thepages/Nakajima.html solar flare cartoon],  
 +
electron acceleration produces beams propagating both downwards and upwards along magnetic field lines. The downwards-going beam propagates along closed loops and produces HXR emission by collisional  
 +
[http://en.wikipedia.org/wiki/Bremsstrahlung bremsstrahlung].  
 +
The signature of the upwards-going beam is a Type III radio burst, which occurs at the local plasma frequency or its harmonics. As the beam propagates away from the sun along open magnetic field lines, it encounters plasma of rapidly decreasing density, so emission occurs at rapidly decreasing frequency, giving Type IIIs a characteristic "hockey stick" shape.  
-
A [http://www.e-callisto.org/ Callisto] radio spectrometer was recently (October 2nd) installed at Glasgow's Acre Road Observatory, as shown in the video, and began observing a few days later. Here we present the [http://www.astro.gla.ac.uk/?page_id=1432 first light observations] and a second burst observed simultaneously by Callisto and RHESSI.
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A [http://www.e-callisto.org/ Callisto] radio spectrometer was recently (October 2nd) installed at Glasgow's  
 +
[http://www.astro.gla.ac.uk/observatory/observ.shtml Acre Road Observatory], and began observing a few days later. Here we present the first-light [http://www.astro.gla.ac.uk/?page_id=1432 observations] and a second burst observed simultaneously by Callisto and RHESSI.
== Type III burst observations with Glasgow Callisto ==
== Type III burst observations with Glasgow Callisto ==
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[[File:Image1.png|thumb|center|400px|supercalifragilisticexpialidocious Figure 1:
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[[File:Image1.png|400px|thumb|center|alt=supercalifragilisticexpialidocious| Figure 1:
The first radio event captured with Glasgow Callisto (with averaged background subtracted) and with Fermi
The first radio event captured with Glasgow Callisto (with averaged background subtracted) and with Fermi
]]
]]
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Figure 1 shows the first light observation, a probable Type III burst, identified by its frequency range and rapid frequency drift. Observations from other sites in the Callisto network help to confirm the identification. RHESSI did not observe this first burst, but X-ray data from the Fermi GBM are available, and are also shown in Figure 1. Simultaneous observations of HXR and Type III emission such as this provide evidence for a common acceleration mechanism for the beams producing the two types, and allow us to infer the properties of the electron accelerator.  
+
Figure 1 shows the first-light observation, a probable Type III burs as identified by its frequency range and rapid frequency drift. Observations from other sites in the Callisto network help to confirm this identification. RHESSI did not observe this first burst, but X-ray data from the  
 +
[http://gammaray.msfc.nasa.gov/gbm/ Fermi Gamma-Ray Burst Monitor] are available, and are also shown in Figure 1. Simultaneous observations of HXR and Type III emission such as this provide evidence for a common acceleration mechanism for the beams producing the two types, and allow us to infer the properties of the electron accelerator.  
[[File:Image2.png|thumb|center|400px|
[[File:Image2.png|thumb|center|400px|
Figure 2:
Figure 2:
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A second Type III event from Glasgow Callisto, with RHESSI count rates and reconstructed image (TO BE ADDED SOON)
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A second Type III event from Glasgow Callisto, with RHESSI count rates
]]
]]
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Slightly over an hour later Glasgow Callisto detected a second burst, also identified as a Type III, for which RHESSI data are available, shown in Figure 2. This event is visible in the 12-25 keV energy band, as well as the lower energies.
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Slightly over an hour later Glasgow Callisto detected a second burst, also identified as a Type III, for which RHESSI data are available, as shown in Figure 2. This event is visible in the 12-25 keV energy band, as well as the lower energies.
== Summary ==
== Summary ==
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The Glasgow Callisto antenna is one part of a larger network, named [http://www.e-callisto.org/ e-Callisto]. Other sites range across the globe, in places including Switzerland, India, Alaska, Australia, Kenya, meaning the network as a whole offers nearly 24 hour observations of the Sun across the entire year. All of the sites suffer some interference from nearby radio sources, including Glasgow. Strong events are visible, such as the two discussed here, and in these cases data from the various locations complement each other.
The Glasgow Callisto antenna is one part of a larger network, named [http://www.e-callisto.org/ e-Callisto]. Other sites range across the globe, in places including Switzerland, India, Alaska, Australia, Kenya, meaning the network as a whole offers nearly 24 hour observations of the Sun across the entire year. All of the sites suffer some interference from nearby radio sources, including Glasgow. Strong events are visible, such as the two discussed here, and in these cases data from the various locations complement each other.
A brief survey of the first 10 days of Glasgow Callisto data show a number of bursts with simultaneous X-ray counterparts, and several without. Comparison with other Callisto sites shows that this is partly due to the Glasgow site missing events which are visible elsewhere, and partly to the relatively low correlation between observed HXR sources, and Type IIIs.  
A brief survey of the first 10 days of Glasgow Callisto data show a number of bursts with simultaneous X-ray counterparts, and several without. Comparison with other Callisto sites shows that this is partly due to the Glasgow site missing events which are visible elsewhere, and partly to the relatively low correlation between observed HXR sources, and Type IIIs.  
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LINKS:
LINKS:
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Characteristics of the flare acceleration region derived from simultaneous hard X-ray and radio observations, [http://adsabs.harvard.edu/abs/2011A%26A...529A..66R here].
Characteristics of the flare acceleration region derived from simultaneous hard X-ray and radio observations, [http://adsabs.harvard.edu/abs/2011A%26A...529A..66R here].
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Glasgow Callisto data and near real time dynamic spectra are [http://www.astro.gla.ac.uk/?page_id=1432 here].
Glasgow Callisto data and near real time dynamic spectra are [http://www.astro.gla.ac.uk/?page_id=1432 here].
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Callisto network data are available [http://soleil.i4ds.ch/solarradio/callistoQuicklooks/ here].
Callisto network data are available [http://soleil.i4ds.ch/solarradio/callistoQuicklooks/ here].
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Anagram key to the Nugget title: "Yapping Mrs Snoop."
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[[Category: Nugget]]

Latest revision as of 12:56, 15 November 2012


Nugget
Number: 187
1st Author: Heather Ratcliffe
2nd Author: Eduard Kontar
Published: 29 October 2012
Next Nugget: Impulse Response
Previous Nugget: Photospheric Temperature


Introduction

Hard X-Ray (HXR) bursts and solar Type III radio bursts are some of the commonest solar emissions caused by energetic electrons. In a well-known solar flare cartoon, electron acceleration produces beams propagating both downwards and upwards along magnetic field lines. The downwards-going beam propagates along closed loops and produces HXR emission by collisional bremsstrahlung. The signature of the upwards-going beam is a Type III radio burst, which occurs at the local plasma frequency or its harmonics. As the beam propagates away from the sun along open magnetic field lines, it encounters plasma of rapidly decreasing density, so emission occurs at rapidly decreasing frequency, giving Type IIIs a characteristic "hockey stick" shape.

A Callisto radio spectrometer was recently (October 2nd) installed at Glasgow's Acre Road Observatory, and began observing a few days later. Here we present the first-light observations and a second burst observed simultaneously by Callisto and RHESSI.

Type III burst observations with Glasgow Callisto

supercalifragilisticexpialidocious
Figure 1: The first radio event captured with Glasgow Callisto (with averaged background subtracted) and with Fermi

Figure 1 shows the first-light observation, a probable Type III burs as identified by its frequency range and rapid frequency drift. Observations from other sites in the Callisto network help to confirm this identification. RHESSI did not observe this first burst, but X-ray data from the Fermi Gamma-Ray Burst Monitor are available, and are also shown in Figure 1. Simultaneous observations of HXR and Type III emission such as this provide evidence for a common acceleration mechanism for the beams producing the two types, and allow us to infer the properties of the electron accelerator.

Figure 2: A second Type III event from Glasgow Callisto, with RHESSI count rates

Slightly over an hour later Glasgow Callisto detected a second burst, also identified as a Type III, for which RHESSI data are available, as shown in Figure 2. This event is visible in the 12-25 keV energy band, as well as the lower energies.

Summary

The Glasgow Callisto antenna is one part of a larger network, named e-Callisto. Other sites range across the globe, in places including Switzerland, India, Alaska, Australia, Kenya, meaning the network as a whole offers nearly 24 hour observations of the Sun across the entire year. All of the sites suffer some interference from nearby radio sources, including Glasgow. Strong events are visible, such as the two discussed here, and in these cases data from the various locations complement each other. A brief survey of the first 10 days of Glasgow Callisto data show a number of bursts with simultaneous X-ray counterparts, and several without. Comparison with other Callisto sites shows that this is partly due to the Glasgow site missing events which are visible elsewhere, and partly to the relatively low correlation between observed HXR sources, and Type IIIs.

LINKS:

Characteristics of the flare acceleration region derived from simultaneous hard X-ray and radio observations, here.

Glasgow Callisto data and near real time dynamic spectra are here.

Callisto network data are available here.

Anagram key to the Nugget title: "Yapping Mrs Snoop."

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