Quiet Sun III

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(New page: {{Infobox Nugget |name = Nugget |title = Quiet Sun III |number = 136 |first_author = Iain Hannah |second_author = Hugh Hudson |publish_date = 2010 September 27 |next_nugget = TBD |previous...)
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|second_author = Hugh Hudson
|second_author = Hugh Hudson
|publish_date = 2010 September 27
|publish_date = 2010 September 27
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|next_nugget = TBD
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|next_nugget = [[Sector Boundaries and RHESSI Flares]]
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|previous_nugget = [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The X-ray Limb]
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|previous_nugget = [[The X-ray Limb]]
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== Introduction ==
== Introduction ==
 +
 +
[[Image:F2.jpg|right|thumb|400px|<b>Figure 1:</b> Upper limits on the hard X-ray emission of the quiet Sun, including historical results and RHESSI data. See reference A for details.]]
Earlier Nuggets, starting in 2005, have explored various facets of
Earlier Nuggets, starting in 2005, have explored various facets of
high-energy radiation from the quiet Sun:
high-energy radiation from the quiet Sun:
-
[http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=16 1],
+
{{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::16]]}}, {{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::21]]}}, {{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::37]]}}, {{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::50]]}}.
-
[http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=21 2],
+
-
[http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=37 3],
+
-
[http://sprg.ssl.berkeley.edu/~tohban/nuggets/?page=article&article_id=50 4].
+
Now we have the definitive RHESSI measurements in hand (reference A), in the
Now we have the definitive RHESSI measurements in hand (reference A), in the
-
sense that the Sun has now passed (with difficulty) a [quite unusual] [solar
+
sense that the Sun has now passed (with difficulty) a quite unusual  
-
minimum], and RHESSI data acquisition for faint exotic hard X-ray emissions
+
[http://en.wikipedia.org/wiki/Solar_variation solar minimum], and RHESSI data acquisition for faint exotic hard X-ray emissions
has come to an end.
has come to an end.
Reference to the earlier Nuggets cited will bring up unusual subjects such as
Reference to the earlier Nuggets cited will bring up unusual subjects such as
-
axions, cosmic-ray electrons, albedo neutrons, and the diffuse cosmic X-ray  
+
cosmic-ray electrons, albedo neutrons, axions, and the diffuse cosmic X-ray  
background.  
background.  
Since RHESSI only obtains upper limits, we cannot say very much about these
Since RHESSI only obtains upper limits, we cannot say very much about these
-
interesting things, except that they are predicted not to be very faint
+
interesting things, except that they are predicted to be very faint,
-
by non-solar astronomical standards.
+
though not by astronomical standards.
-
RHESSI's best observations are now completed, at least for the next few
+
RHESSI's best observations are now completed because of competition from  
-
years, because of competition from increasing [solar activity] (see the  
+
increasing [http://www.scholarpedia.org/article/Solar_activity solar activity] (see the discussion of "nanoflares" below).
-
discussion of "nanoflares" below).
+
-
 
+
-
(Fig. 2 from Hannah et al 2010, upgraded with Edwards & McCracken,
+
-
RESIK, SphinX, and maybe XRT data if I can interpret them)
+
== The new data ==
== The new data ==
Line 41: Line 36:
In Reference A we describe the full observing program for faint global
In Reference A we describe the full observing program for faint global
hard X-ray emission from the Sun.
hard X-ray emission from the Sun.
-
We have not made any great discovery - no axions yet - but
+
It has resulted in better upper limits rather than in a positive
-
the RHESSI data have provided the best upper limits to date (Figure 1).
+
detection (see Figure 1).
-
Until focusing optics, such as those of [Nustar] or [FOXSI] become available,
+
Not only does RHESSI not detect any of the more exotic possible
-
these are the best hard X-ray data.
+
sources; these limits also exclude low levels of "normal" magnetic
-
 
+
activity.
-
(Figure from the Sylwester EOS article?)
+
We discuss this latter result the "Nanoflares" section below.
-
This is the final statement from RHESSI on this topic owing to the
+
Until focusing optics, such as those of [http://www.nustar.caltech.edu/ NuSTAR]
 +
or [http://cat.inist.fr/?aModele=afficheN&cpsidt=22321055 FOXSI] become available,
 +
these are the best hard X-ray data.
 +
Figure 1 is the final statement from RHESSI on this topic owing to the
increase of [solar activity].
increase of [solar activity].
-
Other recent instruments (e.g., [SphinX]) or [MESSENGER] may improve
+
Other recent instruments  
 +
(e.g., [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The_SphinX_Instrument_on_CORONAS-PHOTON SphinX])  
 +
or [http://messenger.jhuapl.edu/ MESSENGER] may improve
on these limits, especially at lower energies, and we encourage the analysis
on these limits, especially at lower energies, and we encourage the analysis
of such data on the quiet Sun.
of such data on the quiet Sun.
As discussed below high spectral resolution may be very important in  
As discussed below high spectral resolution may be very important in  
this domain, as well as good background rejection, to distinguish  
this domain, as well as good background rejection, to distinguish  
-
exotic sources from the expected thermal signatures (see next section).
+
exotic sources from the expected magnetic signatures (see next section).
== Nanoflares ==
== Nanoflares ==
-
But the Sun has a continuous level of [magnetic activity], culminating in
+
[[Image:136fig2.jpg|left|thumb|400px|<b>Figure 2:</b> The possible contributions of normal coronal activity to the hard X-ray spectrum.]]
-
sunspots, plage, flares, and CMEs.
+
 
-
In particular [nanoflares] are an attractive scenario that might
+
The Sun has a continuous but variable level of  
-
solve the [coronal heating] problem.
+
[http://www.scholarpedia.org/article/Solar_activity solar magnetic activity], seen for
 +
example as [http://en.wikipedia.org/wiki/Plage_(astronomy) plage],  
 +
[http://www.google.com/images?client=safari&rls=en&q=solar+flare&oe=UTF-8&um=1&ie=UTF-8&source=univ&ei=pOehTNKHEpK6sQP237h7&sa=X&oi=image_result_group&ct=title&resnum=6&ved=0CEoQsAQwBQ&biw=1056&bih=647 flares],  
 +
and [http://www.windows2universe.org/sun/cmes.html CMEs].
 +
There is a hot [http://imagine.gsfc.nasa.gov/docs/science/mysteries_l1/corona.html corona], brightest in sunspot regions, and in
 +
a well-known theory [http://en.wikipedia.org/wiki/Eugene_Parker Parker] suggested that "nanoflares" - tiny
 +
non-thermal energy releases, undetectable individually but very numerous,
 +
could merge together and explain the heating needed.
In essence the nanoflare hypothesis involves episodic heating, perhaps
In essence the nanoflare hypothesis involves episodic heating, perhaps
resembling the action of true solar flares; to support a mean coronal
resembling the action of true solar flares; to support a mean coronal
-
temperature means that impulsive nanoflare heating would produce  
+
temperature means mathematically that impulsive nanoflare heating  
-
temperatures higher than the mean.
+
would produce temperatures higher than the mean.
In other words, the instantaneous temperature distribution of the
In other words, the instantaneous temperature distribution of the
corona would be broader than for a steady heating process that only
corona would be broader than for a steady heating process that only
has to attain the mean coronal temperature.
has to attain the mean coronal temperature.
-
This kind of process therefore competes in an ill-understood manner
+
If the nanoflares were physically similar to ordinary flares, we
-
with our search for faint hard X-ray sources not related to solar
+
would also expect bursts of hard X-ray bremsstrahlung (see Reference [A]).
-
magnetic activity.
+
This component of quiet-Sun emission should be detectable by an
-
It is also interesting in its own right and the subject of a great deal
+
appropriately sensitive measurement.
-
of literature (e.g. ref. [2]).
+
See reference [B] for fuller background.
 +
 
 +
[[Image:136fig3.jpg|right|thumb|350px|<b>Figure 3:</b> Time-series photometry of the truly quiet Sun, as recorded by [http://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/The_SphinX_Instrument_on_CORONAS-PHOTON SphinX].]]
 +
 
 +
In Figure 3 we show recent observations from the SphinX experiment.
 +
It makes sensitive soft X-ray observations with spectral resolution
 +
somewhat better than RHESSI's, and greatly improves on the standard
 +
[GOES] soft X-ray data.
 +
The point of this figure is that the data show periods of quiet coronal
 +
emission, with no flares; even during the presence of active regions,
 +
there are apparently steady emission levels.  
 +
This absence of flare-like variation suggests that the physics of
 +
nanoflares, if they exist, is quite different from that of flares.
 +
The real test will be in the spectroscopy, ie in the search for
 +
significant broadening of the temperature distribution away from
 +
the mean..
 +
 
-
(Fig. 3 left from Hannah et al 2010)
 
== Conclusions ==
== Conclusions ==
Line 84: Line 106:
RHESSI cannot improve on these limits for another several years,
RHESSI cannot improve on these limits for another several years,
and there are no plans now for new and more sensitive hard X-ray
and there are no plans now for new and more sensitive hard X-ray
-
solar instrumentation (but we look forward to [FOXSI] and [NuSTAR]).
+
solar instrumentation (but we look forward to FOXSI and NuSTAR).
These limits may stand as definitive ones for some time to come.
These limits may stand as definitive ones for some time to come.
In the meanwhile it is important to study the 1-10 keV range with
In the meanwhile it is important to study the 1-10 keV range with
available data.
available data.
 +
Because the thermal spectra are steep, spectroscopic observations
 +
are important.
== References ==
== References ==
-
[1] Hannah et al
+
[A] [http://arxiv.org/abs/1009.2918 "Constraining the hard X-ray properties of the quiet sun with new RHESSI observations"]
 +
 
 +
[B] [http://arxiv.org/abs/astro-ph/0511841 "On solving the coronal heating problem"]
-
[2] Klimchuk review
+
[[Category: Nugget]]

Latest revision as of 17:24, 23 August 2018


Nugget
Number: 136
1st Author: Iain Hannah
2nd Author: Hugh Hudson
Published: 2010 September 27
Next Nugget: Sector Boundaries and RHESSI Flares
Previous Nugget: The X-ray Limb
List all



Contents

Introduction

Figure 1: Upper limits on the hard X-ray emission of the quiet Sun, including historical results and RHESSI data. See reference A for details.

Earlier Nuggets, starting in 2005, have explored various facets of high-energy radiation from the quiet Sun: Exploring the Quiet Sun 1, A Solar Hard X-Ray Halo: Exploring the Quiet Sun 2, Solar radiation belts?, Solar X-rays from axions. Now we have the definitive RHESSI measurements in hand (reference A), in the sense that the Sun has now passed (with difficulty) a quite unusual solar minimum, and RHESSI data acquisition for faint exotic hard X-ray emissions has come to an end.

Reference to the earlier Nuggets cited will bring up unusual subjects such as cosmic-ray electrons, albedo neutrons, axions, and the diffuse cosmic X-ray background. Since RHESSI only obtains upper limits, we cannot say very much about these interesting things, except that they are predicted to be very faint, though not by astronomical standards. RHESSI's best observations are now completed because of competition from increasing solar activity (see the discussion of "nanoflares" below).

The new data

In Reference A we describe the full observing program for faint global hard X-ray emission from the Sun. It has resulted in better upper limits rather than in a positive detection (see Figure 1). Not only does RHESSI not detect any of the more exotic possible sources; these limits also exclude low levels of "normal" magnetic activity. We discuss this latter result the "Nanoflares" section below.

Until focusing optics, such as those of NuSTAR or FOXSI become available, these are the best hard X-ray data. Figure 1 is the final statement from RHESSI on this topic owing to the increase of [solar activity]. Other recent instruments (e.g., SphinX) or MESSENGER may improve on these limits, especially at lower energies, and we encourage the analysis of such data on the quiet Sun. As discussed below high spectral resolution may be very important in this domain, as well as good background rejection, to distinguish exotic sources from the expected magnetic signatures (see next section).

Nanoflares

Figure 2: The possible contributions of normal coronal activity to the hard X-ray spectrum.

The Sun has a continuous but variable level of solar magnetic activity, seen for example as plage, flares, and CMEs. There is a hot corona, brightest in sunspot regions, and in a well-known theory Parker suggested that "nanoflares" - tiny non-thermal energy releases, undetectable individually but very numerous, could merge together and explain the heating needed. In essence the nanoflare hypothesis involves episodic heating, perhaps resembling the action of true solar flares; to support a mean coronal temperature means mathematically that impulsive nanoflare heating would produce temperatures higher than the mean. In other words, the instantaneous temperature distribution of the corona would be broader than for a steady heating process that only has to attain the mean coronal temperature. If the nanoflares were physically similar to ordinary flares, we would also expect bursts of hard X-ray bremsstrahlung (see Reference [A]). This component of quiet-Sun emission should be detectable by an appropriately sensitive measurement. See reference [B] for fuller background.

Figure 3: Time-series photometry of the truly quiet Sun, as recorded by SphinX.

In Figure 3 we show recent observations from the SphinX experiment. It makes sensitive soft X-ray observations with spectral resolution somewhat better than RHESSI's, and greatly improves on the standard [GOES] soft X-ray data. The point of this figure is that the data show periods of quiet coronal emission, with no flares; even during the presence of active regions, there are apparently steady emission levels. This absence of flare-like variation suggests that the physics of nanoflares, if they exist, is quite different from that of flares. The real test will be in the spectroscopy, ie in the search for significant broadening of the temperature distribution away from the mean..


Conclusions

This Nugget reports the best upper limits on hard X-rays from the quiet Sun, including several possible mechanisms. RHESSI cannot improve on these limits for another several years, and there are no plans now for new and more sensitive hard X-ray solar instrumentation (but we look forward to FOXSI and NuSTAR). These limits may stand as definitive ones for some time to come. In the meanwhile it is important to study the 1-10 keV range with available data. Because the thermal spectra are steep, spectroscopic observations are important.

References

[A] "Constraining the hard X-ray properties of the quiet sun with new RHESSI observations"

[B] "On solving the coronal heating problem"

Retrieved from "https://sprg.ssl.berkeley.edu/~tohban/wiki/index.php/Quiet_Sun_III"
Facts about Quiet Sun IIIRDF feed
RHESSI Nugget Date27 September 2010  +
RHESSI Nugget First AuthorIain Hannah  +
RHESSI Nugget Index136  +
RHESSI Nugget Second AuthorHugh Hudson  +
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