The Marshall Grazing Incidence X-ray Spectrograph (MaGIXS)

Kobayashi, K.; Cirtain, Jonathan; Golub, L.; Winebarger, Amy R.; Hertz, Edward; Cheimets, Peter; Caldwell, David; Korreck, K. E.; Robinson, B.; Reardon, Patrick J.; Kester, Thomas; Griffith, Charles W.; Young, Mark

doi:10.1117/12.894071

Cited by 14 publications

(8 citation statements)

References 6 publications

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“…These observations would greatly benefit from new, more sensitive, solar X-ray telescopes such as the FOXSI (Krucker et al 2014) and MaGIXS (Kobayashi et al 2011) sounding rockets, as well as the MinXSS CubeSats (Mason et al 2016). New data combined with NuSTAR observations during quieter periods of solar activity should provide detection of the hightemperature and possible non-thermal emission in even smaller microflares, which should, in turn, provide a robust measure of their contribution to heating coronal loops in ARs.…”

Section: Discussionmentioning

confidence: 99%

Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA

Wright

Hannah

Grefenstette

et al. 2017

ApJ

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NuSTAR is a highly sensitive focusing hard X-ray (HXR) telescope and has observed several small microflares in its initial solar pointings. In this paper, we present the first joint observation of a microflare with NuSTAR and Hinode/ XRT on 2015 April 29 at ∼11:29 UT. This microflare shows the heating of material to several million Kelvin, observed in soft X-rays with Hinode/XRT, and was faintly visible in the extreme ultraviolet with SDO/AIA. For three of the four NuSTAR observations of this region (pre-flare, decay, and post-flare phases), the spectrum is well fitted by a single thermal model of 3.2-3.5 MK, but the spectrum during the impulsive phase shows additional emission up to 10 MK, emission equivalent to the A0.1 GOES class. We recover the differential emission measure (DEM) using SDO/AIA, Hinode/XRT, and NuSTAR, giving unprecedented coverage in temperature. We find that the pre-flare DEM peaks at ∼3 MK and falls off sharply by 5 MK; but during the microflare's impulsive phase, the emission above 3 MK is brighter and extends to 10 MK, giving a heating rate of about2.5 10 25 erg s −1. As the NuSTAR spectrum is purely thermal, we determined upper limits on the possible non-thermal bremsstrahlung emission. We find that for the accelerated electrons to be the source of heating, a power-law spectrum of  d 7 with a low-energy cutoff  E 7 c keV is required. In summary, this first NuSTAR microflare strongly resembles much more powerful flares.

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Section: Discussionmentioning

confidence: 99%

Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA

Wright

Hannah

Grefenstette

et al. 2017

ApJ

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“…Future measurements from the Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) (Kobayashi et al. , 2011 ) sounding rocket and continued measurements from the Focusing Optics X-ray Solar Imager (FOXSI: Ishikawa et al. , 2014 ) sounding rockets as well as the NuSTAR satellite (Hannah et al.…”

Section: Minxss-1 Solar Measurements From Goes A5–m5 Levelsmentioning

confidence: 99%

The Instruments and Capabilities of the Miniature X-Ray Solar Spectrometer (MinXSS) CubeSats

et al. 2018

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The Miniature X-ray Solar Spectrometer (MinXSS) CubeSat is the first solar science oriented CubeSat mission flown for the NASA Science Mission Directorate, with the main objective of measuring the solar soft X-ray (SXR) flux and a science goal of determining its influence on Earth’s ionosphere and thermosphere. These observations can also be used to investigate solar quiescent, active region, and flare properties. The MinXSS X-ray instruments consist of a spectrometer, called X123, with a nominal 0.15 keV full-width at half-maximum (FWHM) resolution at 5.9 keV and a broadband X-ray photometer, called XP. Both instruments are designed to obtain measurements from 0.5 – 30 keV at a nominal time cadence of 10 s. A description of the MinXSS instruments, performance capabilities, and relation to the Geostationary Operational Environmental Satellite (GOES) 0.1 – 0.8 nm flux is given in this article. Early MinXSS results demonstrate the capability of measuring variations of the solar spectral soft X-ray (SXR) flux between 0.8 – 12 keV from at least GOES A5–M5 ( ) levels and of inferring physical properties (temperature and emission measure) from the MinXSS data alone. Moreover, coronal elemental abundances can be inferred, specifically for Fe, Ca, Si, Mg, S, Ar, and Ni, when the count rate is sufficiently high at each elemental spectral feature. Additionally, temperature response curves and emission measure loci demonstrate the MinXSS sensitivity to plasma emission at different temperatures. MinXSS observations coupled with those from other solar observatories can help address some of the most compelling questions in solar coronal physics. Finally, simultaneous observations by MinXSS and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) can provide the most spectrally complete soft X-ray solar flare photon flux measurements to date.

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“…The spectrum was calculated with the CHIANTI package (Dere et al, 1997;Del Zanna et al, 2015). Kobayashi et al, 2011;Siarkowski et al, 2016). We propose to use three different instruments for three different spectral lines.…”

Section: New Spectral Channelsmentioning

confidence: 99%

“…Imaging spectrometers-such as the Extreme ultraviolet Imaging Spectrometer (Culhane et al, 2007) on board the Hinode satellite (Kosugi et al, 2007), the Coronal Diagnostic Spectrometer (Harrison et al, 1995) on board the Solar and Heliospheric Observatory (Domingo et al, 1995), the Interface Region Imaging Spectrograph (De Pontieu et al, 2014), or Marshall Grazing Incidence X-ray Spectrometer (MaGIXS; Kobayashi et al, 2011;Athiray et al, 2019)-can achieve this goal. These instruments build raster images of the solar corona in multiple spectral lines.…”

Section: Introductionmentioning

confidence: 99%

Monochromatic X-Ray Imagers of the Sun Based on the Bragg Crystal Optics

Reva

Kuzin

Кириченко

et al. 2021

Front. Astron. Space Sci.

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Investigations of solar activity require information about plasma in a wide range of temperatures. Generally, researchers require observations from telescopes producing monochromatic images of coronal plasma with cool, warm, and hot temperatures. Until now, monochromatic telescopic imaging has been made only in the Mg XII 8.42 Å line with the Mg XII spectroheliograph on board CORONAS-I, CORONAS-F, and CORONAS-PHOTON satellites. The Mg XII spectroheliograph used Bragg crystal optics. Its design is based on two main principles: (1) to select the working wavelength and the crystal in such a way that reflection occurs at small incident angles; (2) to use the aperture of the mirror as a spectral filter. We believe that these design principles can be applied to other spectral lines. In this article, we will review the design of the Mg XII spectroheliograph and present our thoughts on how to apply these principles to the Si XIV 6.18 Å and Si XIII 6.65 Å lines. A combination of the monochromatic Mg XII 8.42 Å, Si XIV 6.18 Å, and Si XIII 6.65 Å images will help us to study the dynamics of the hot plasma in the solar corona.

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The Marshall Grazing Incidence X-ray Spectrograph (MaGIXS)

Cited by 14 publications

References 6 publications

Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA

Microflare Heating of a Solar Active Region Observed with NuSTAR, Hinode/XRT, and SDO/AIA

The Instruments and Capabilities of the Miniature X-Ray Solar Spectrometer (MinXSS) CubeSats

Monochromatic X-Ray Imagers of the Sun Based on the Bragg Crystal Optics

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