The Sun and heliosphere explorer – the Interhelioprobe mission

Кузнецов, В. Д.; Zelenyǐ, L. M.; Zimovets, I. V.; Anufreychik, Konstantin; Безруких, В. В.; Chulkov, I.; Коновалов, А. А.; Котова, Г. А.; Kovrazhkin, R. A.; Moiseenko, D. A.; Petrukovich, A. A.; Remizov, A. P.; Shestakov, A.; Skalsky, A.; Вайсберг, О. Л.; Веригин, М. И.; Zhuravlev, R. N.; Andreevskyi, S. E.; Dokukin, V. S.; Фомичев, В. В.; Lebedev, N. I.; Обридко, В. Н.; Polyanskyi, V. P.; Styazhkin, V. A.; Rudenchik, E. A.; Sinelnikov, V. M.; Zhugzhda, Y. D.; Ryzhenko, A. P.; Иванов, А. В.; Simonov, A. V.; Dobrovolskyi, V. S.; Konstantinov, M. S.; Kuzin, S. V.; Богачев, С. А.; Kholodilov, A. A.; Кириченко, А. М.; Lavrentiev, E. N.; Pertsov, A. A.; Reva, A. A.; Shestov, S. V.; Ulyanov, A. S.; Panasyuk, M. I.; Iyudin, A. F.; Свертилов, С. И.; Bogomolov, V. V.; Галкин, В. И.; Marjin, B. V.; Morozov, O. V.; Оседло, В. И.; Rubinshtein, I. A.; Scherbovsky, B. Ya.; Tulupov, V. I.; Kotov, Yu. D.; Yurov, V. N.; Glyanenko, A. S.; Kochemasov, A. V.; Lupar, E. E.; Rubtsov, Igor V.; Trofimov, Yu. A.; Tyshkevich, V. G.; Улин, С. Е.; Novikov, Alexander; Дмитренко, В. В.; Grachev, V. M.; Stekhanov, V.; Власик, К. Ф.; Uteshev, Z. M.; Chernysheva, I. V.; Shustov, A.; Petrenko, D; Aptekar, R.; Dergachev, V. A.; Golenetskii, S.; Gribovskyi, K. S.; Frederiks, D.; Kruglov, E. M.; Lazutkov, V. P.; Levedev, V. V.; Oleinik, F. P.; Pal'Shin, V.; Repin, A. I.; Savchenko, M. I.; Skorodumov, D. V.; Svinkin, D.; Tsvetkova, A. E.; Ulanov, M.; Kozhevatov, I. E.; Sylwester, J.; Siarkowski, M.; Bakala, Jaroslaw; Szaforz, Żaneta; Kowaliński, Mirosław; Dudnik, O. V.; Lavraud, B.; Hruška, František; Kolmašová, Ivana; Santolı́k, O.; Šimůnek, Jiřı́; Truhlík, Vladimír; Auster, H-U.; Hilchenbach, M.; Venedictov, Yu.; Berghofer, G.

doi:10.1134/s0016793216070124

Cited by 23 publications

(5 citation statements)

References 87 publications

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“…We think that monochromatic imagers similar to the Mg XII spectroheliograph-for example, see Kuznetsov et al (2016), Kirichenko et al (2021), andReva et al (2021)-can help us study reconnection heating. We hope that such instruments will be created in the future and that they will improve our understanding of the processes occurring inside the current sheets during solar flares.…”

Section: Discussionmentioning

confidence: 99%

Observations of Current Sheet Heating in X-Ray during a Solar Flare

Reva

Богачев

Loboda

et al. 2022

ApJ

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In the solar corona, magnetic reconnection occurs due to the finite resistivity of the plasma. At the same time, this resistivity leads to ohmic heating. Therefore, the reconnecting current sheet should heat the surrounding plasma. This paper presents experimental evidence of such plasma heating being caused by magnetic reconnection. We observed the effect during a C1.4 solar flare on 2003 February 16 at the active region NOAA 10278, near the solar limb. Thanks to such a location, we successfully identified all the principal elements of the flare: the flare arcade, the flux rope, and, most importantly, the presumed position of the current sheet. By analyzing the monochromatic X-ray images of the Sun obtained by the CORONAS-F/SPIRIT instrument in the Mg xii 8.42 Å spectral line, we detected a high-temperature (T ≥ 4 MK) emission at the predicted location of the current sheet. The high-temperature emission appeared during the CME’s impulsive acceleration phase. We believe that this additionally confirms that the plasma heating around the current sheet and the magnetic reconnection inside the current sheet are strongly connected.

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Section: Discussionmentioning

confidence: 99%

Observations of Current Sheet Heating in X-Ray during a Solar Flare

Reva

Богачев

Loboda

et al. 2022

ApJ

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“…Currently, the interest to the soft X-ray spectral range is revitalizing. The upcoming ChemiX instrument on board the Interhelioprobe satellite will register full Sun spectra in the range of 1.5-8.8 Å (Kuznetsov et al, 2016;Siarkowski et al, 2016). Marshall Grazing Incidence X-ray Spectrometer (MaGIXS) is an upcoming rocket flight experiment, which will perform stigmatic imaging spectroscopy in the 6-24 Å spectral range (Kobayashi et al, 2011;Athiray et al, 2019).…”

Section: Discussionmentioning

confidence: 99%

“…The Mg XII spectroheliograph operated on board CORONAS-I (Sobel' Man et al, 1996), CORONAS-F (Zhitnik et al, 2002(Zhitnik et al, , 2003aZhithik et al, 2005), and CORONAS-PHOTON satellites (Kotov, 2011;Kuzin et al, 2011). The instrument is a part of the future missions such as Interhelioprobe (Kuznetsov et al, 2016) and KORTES (Shestov et al, 2014). Below we will briefly review these missions.…”

Section: Mg XII Spectroheliographmentioning

confidence: 99%

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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 instruments to be flown are: a full-disk vector magnetograph, Lyman-α imaging telescopes covering both the disk and corona, a full-disk white light telescope, and a hard X-ray imaging telescope. The Solar and Heliosphere Explorer-also known as Interhelioprobe-is a Russian mission consisting of two identical spacecraft expected to be launched in the 2026-27 timeframe (Kuznetsov et al, 2016). The mission profile is similar to the European Space Agency's Solar Orbiter, with the spacecraft reaching as close as 0.3 AU to the Sun and up to 30 • above the ecliptic plane.…”

Section: Non-us Solar Missionsmentioning

confidence: 99%

Future Prospects for Solar EUV and Soft X-Ray Spectroscopy Missions

Young

2021

Front. Astron. Space Sci.

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Future prospects for solar spectroscopy missions operating in the extreme ultraviolet (EUV) and soft X-ray (SXR) wavelength ranges, 1.2–1,600 Å, are discussed. NASA is the major funder of Solar Physics missions, and brief summaries of the opportunities for mission development under NASA are given. Upcoming major solar missions from other nations are also described. The methods of observing the Sun in the two wavelength ranges are summarized with a discussion of spectrometer types, imaging techniques and detector options. The major spectral features in the EUV and SXR regions are identified, and then the upcoming instruments and concepts are summarized. The instruments range from large spectrometers on dedicated missions, to tiny, low-cost CubeSats launched through rideshare opportunities.

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The Sun and heliosphere explorer – the Interhelioprobe mission

Cited by 23 publications

References 87 publications

Observations of Current Sheet Heating in X-Ray during a Solar Flare

Observations of Current Sheet Heating in X-Ray during a Solar Flare

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

Future Prospects for Solar EUV and Soft X-Ray Spectroscopy Missions

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