Remembering Marcos Machado via his research
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|name = Nugget | |name = Nugget | ||
|title = Remembering Marcos Machado via his research | |title = Remembering Marcos Machado via his research | ||
- | |number = | + | |number = 336 |
|first_author = Hugh Hudson | |first_author = Hugh Hudson | ||
|second_author = | |second_author = | ||
|publish_date = 12 November 2018 | |publish_date = 12 November 2018 | ||
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- | |previous_nugget={{#ask: [[Category:Nugget]] [[RHESSI Nugget Index:: | + | |previous_nugget={{#ask: [[Category:Nugget]] [[RHESSI Nugget Index::335]]}} |
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== Introduction == | == Introduction == | ||
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Marcos Machado, an old friend and colleague, passed away in September, | Marcos Machado, an old friend and colleague, passed away in September, | ||
2018, much to our sorrow. | 2018, much to our sorrow. | ||
+ | Please see the further detail in the | ||
+ | [http://spd.stanford.edu//SolarNews/2018/20181001.html#section_mandrini obituary] | ||
+ | written by his first PhD student, | ||
+ | [https://www.iau.org/administration/membership/individual/1216/ Cristina Mandrini]. | ||
- | Marcos and I shared common interests but very different backgrounds | + | Marcos and I shared common interests but had very different backgrounds |
- | - he, as an astronomer, actually | + | - he, as an astronomer, actually understood radiative-transfer theory. |
Thus I (best defined then as a cosmic-ray physicist) learned a great | Thus I (best defined then as a cosmic-ray physicist) learned a great | ||
deal about how solar flares work from him, and his great work from | deal about how solar flares work from him, and his great work from | ||
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We are very fortunate that at the end he again had enthusiastically | We are very fortunate that at the end he again had enthusiastically | ||
embraced flare research, specifically re-visiting his early work | embraced flare research, specifically re-visiting his early work | ||
- | in EUV astronomy -but now using the very precise [SDO/EVE] data, | + | in EUV astronomy - but now using the very precise |
- | which give Sun-as-a-star views of the EUV, a most crucial spectral | + | [http://lasp.colorado.edu/home/missions-projects/quick-facts-sdo-eve/ SDO/EVE] data, |
- | band since it shows us the behavior of the [transition region] of | + | which give Sun-as-a-star views of the |
- | the solar atmosphere, though without imaging. Ref. [2] captures | + | [https://en.wikipedia.org/wiki/Extreme_ultraviolet EUV], a most crucial spectral |
- | this work, published posthumously thanks to Ryan Milligan and Paulo | + | band since it shows us the behavior of the |
- | + | [https://en.wikipedia.org/wiki/Solar_transition_region transition region] of | |
+ | the solar atmosphere, though without imaging. | ||
+ | |||
+ | Ref. [2] captures this work, published posthumously thanks to Ryan | ||
+ | Milligan and Paulo Simões. | ||
+ | It comes just 40 years after Ref. [3], a work of major significance on | ||
+ | the very same topic, published during Marcos's postdoctoral stay | ||
+ | at Harvard. | ||
+ | Note that this was actually the same institution in which | ||
+ | [https://en.wikipedia.org/wiki/Theodore_Lyman Lyman] identified | ||
+ | these features early in the 20th century. | ||
== The Lyman Continuum == | == The Lyman Continuum == | ||
- | The new work examines the behavior of the [Lyman | + | The new work examines the behavior of the |
+ | [https://en.wikipedia.org/wiki/Lyman_continuum_photons Lyman continuum] in a | ||
representative set of strong solar flares. | representative set of strong solar flares. | ||
- | As the basic continuum emission (the | + | As the basic continuum emission (recombination to the ground state) of the most |
abundant element (in the nearest star) this spectral feature cries | abundant element (in the nearest star) this spectral feature cries | ||
- | out for deep understanding. | + | out for deep and detailed understanding. |
Figure 1 shows some EVE data. | Figure 1 shows some EVE data. | ||
In thermal equilibrium, the population of the excited level | In thermal equilibrium, the population of the excited level | ||
should reflect the kinetic temperature of the electrons in the | should reflect the kinetic temperature of the electrons in the | ||
- | plasma, and indeed its slope approximates a [Planck | + | plasma, and indeed its slope approximates a blackbody |
+ | [https://en.wikipedia.org/wiki/Max_Planck Planck] function | ||
that reflects the physical temperature in the region around | that reflects the physical temperature in the region around | ||
[optical depth] unity. | [optical depth] unity. | ||
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]] | ]] | ||
- | As shown in Ref. [ | + | As shown in Ref. [4], the continuum irradiance detected by EVE should |
vary as | vary as | ||
- | [[File:336f1.png| | + | [[File:336f1.png|300px|thumb|center |
]] | ]] | ||
relating the EVE irradiance F to the Planck function, as modified by | relating the EVE irradiance F to the Planck function, as modified by | ||
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The very nice paper (Ref. [2]) that Ryan and Paulo helped Marcos to | The very nice paper (Ref. [2]) that Ryan and Paulo helped Marcos to | ||
complete really confirms some of Marcos's early work, with the | complete really confirms some of Marcos's early work, with the | ||
- | very limited [Skylab] data. | + | very limited [https://en.wikipedia.org/wiki/Apollo_Telescope_Mount Skylab] data. |
- | It also extends it because EVE gave access to | + | It also extends it because EVE gave access to the remarkably |
powerful flare, SOL2017-09-06. | powerful flare, SOL2017-09-06. | ||
We greatly regret the loss of a friend but also the re-awakened | We greatly regret the loss of a friend but also the re-awakened | ||
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== References == | == References == | ||
- | [1] [http://adsabs.harvard.edu/abs/1975SoPh...42..395M " | + | [1] [http://adsabs.harvard.edu/abs/1975SoPh...42..395M "Flare model chromospheres and photospheres"] |
+ | |||
+ | [2] [http://adsabs.harvard.edu/cgi-bin/bib_query?arXiv:1810.10824 "Lyman continuum observations of solar flares using SDO/EVE"] | ||
- | [ | + | [3] [http://adsabs.harvard.edu/abs/1978SoPh...59..129M "Lyman continuum observations of solar flares"] |
- | [ | + | [4] [http://adsabs.harvard.edu/abs/1970SoPh...15..120N "The Solar Lyman Continuum and the Structure of the Solar Chromosphere"] |
Latest revision as of 20:14, 7 December 2018
Nugget | |
---|---|
Number: | 336 |
1st Author: | Hugh Hudson |
2nd Author: | |
Published: | 12 November 2018 |
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Contents |
Introduction
Marcos Machado, an old friend and colleague, passed away in September, 2018, much to our sorrow. Please see the further detail in the obituary written by his first PhD student, Cristina Mandrini.
Marcos and I shared common interests but had very different backgrounds - he, as an astronomer, actually understood radiative-transfer theory. Thus I (best defined then as a cosmic-ray physicist) learned a great deal about how solar flares work from him, and his great work from his first active period as a scientist included a really good stab at defining the solar atmosphere during the impulsive phase of a flare (Ref. [1]). Later great works involved solar X-ray astronomy, and then (to our regret) he moved into administrative work.
We are very fortunate that at the end he again had enthusiastically embraced flare research, specifically re-visiting his early work in EUV astronomy - but now using the very precise SDO/EVE data, which give Sun-as-a-star views of the EUV, a most crucial spectral band since it shows us the behavior of the transition region of the solar atmosphere, though without imaging.
Ref. [2] captures this work, published posthumously thanks to Ryan Milligan and Paulo Simões. It comes just 40 years after Ref. [3], a work of major significance on the very same topic, published during Marcos's postdoctoral stay at Harvard. Note that this was actually the same institution in which Lyman identified these features early in the 20th century.
The Lyman Continuum
The new work examines the behavior of the Lyman continuum in a representative set of strong solar flares. As the basic continuum emission (recombination to the ground state) of the most abundant element (in the nearest star) this spectral feature cries out for deep and detailed understanding. Figure 1 shows some EVE data. In thermal equilibrium, the population of the excited level should reflect the kinetic temperature of the electrons in the plasma, and indeed its slope approximates a blackbody Planck function that reflects the physical temperature in the region around [optical depth] unity.
Figure 2 contrasts the Lyman continuum spectral parameters for the gradual and impulsive phases of SOL2017-09-06. The extremely high color temperature in the impulsive-phase spectrum (right) probably sets a record. Is it because the continuum now forms above the height of hydrogen temperature regulation, or is it a reflection of non-thermal physics?
As shown in Ref. [4], the continuum irradiance detected by EVE should vary as
relating the EVE irradiance F to the Planck function, as modified by the b1 "departure coefficient" and the angular subtense of the flare. The departure coefficient here is the ratio of the population of the first excited state of hydrogen, normalized to the value expected in thermal equilibrium. But the theory assumes Maxwellian distributions throughout, of course, and in the impulsive phase of a flare we certainly could have non-equilibrium processes at work.
Conclusion
The very nice paper (Ref. [2]) that Ryan and Paulo helped Marcos to complete really confirms some of Marcos's early work, with the very limited Skylab data. It also extends it because EVE gave access to the remarkably powerful flare, SOL2017-09-06. We greatly regret the loss of a friend but also the re-awakened leadership he demonstrated in this wonderful observation. It points the way to what we could learn from the Lyman continuum if only we had imaging spectroscopy to augment EVE's temporal resolution. In the meanwhile we must rely upon a combination of intuition and modeling, still in the style Marcos brought to this subject many decades ago.
References
[1] "Flare model chromospheres and photospheres"
[2] "Lyman continuum observations of solar flares using SDO/EVE"
[3] "Lyman continuum observations of solar flares"
[4] "The Solar Lyman Continuum and the Structure of the Solar Chromosphere"
RHESSI Nugget Date | 12 November 2018 + |
RHESSI Nugget First Author | Hugh Hudson + |
RHESSI Nugget Index | 336 + |