DOCSLIB.ORG

The SOHO Extreme Ultraviolet Imaging Telescope the EIT

Total Page：16

File Type：pdf, Size：1020Kb

Download full-text PDF Read full-text
The SOHO Extreme Ultraviolet Imaging Telescope the EIT SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 1 of 9 The SOHO Extreme ultraviolet Imaging Telescope brought to you by The EIT Consortium End of SOHO EIT CME watch observations At the end of 2010 July, SOHO's Extreme ultraviolet Imaging Telescope (EIT) will complete fourteen and a half years of synoptic observations of the low corona. SDO AIA images at much higher resolution and time cadence are now available for all the EIT wavebands, and three other EUV wavelengths as well. The telemetry bandwidth that has been used by EIT will be used by LASCO to improve the cadence of its observations of the fastest CME's. EIT will continue to obtain a couple of "synoptic sets" of images in all four wavelengths per day to track detector behavior, and to maintain the uniform data set. This, and other changes in SOHO instrument operations, are part of the transition to the "Bogart" phase of the SOHO mission — designed to get the maximum science out of the mission at the minimum cost to NASA's shrinking Heliophysics Mission Operations and Data Analysis (MO&DA) budget. EIT data will continue to be available via the Virtual Solar Observatory and via the older EIT Web catalog interface. |Skip navigation bar | New EIT synoptic charts | An EIT campaign of high cadence observations in shutterless readout mode | EIT observations in support of the total solar eclipses | Web access to EIT images and FITS files | EIT calibration rocket | EIT 195 Å movies of a disk CME | EIT 195 Å/171 Å temperature diagnostic maps | EIT Observing Targets | EIT Science Topics | Current Solar Images | EIT Observing Programs | What EIT is Designed to Do | The Instrument | Response: Updated Daily | Response: EIT CCD bakeout history | EIT detector response to SEP events | Engineering: EIT Temperature Plots | Engineering: http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 2 of 9 LASCO OBE software load history | Data Rights Policy | Science Planning Schedule | EIT User's Handbook | Operations Team | SDAC Home | SOHO Home | EIT User's Handbook , EIT Calibration, EIT software updates occur on December 10, 2001. Accessing EIT data If you want GIF images of EIT data.... You can find both the latest, full-field EIT images, and earlier image (EIT and other) in the SOHO summary database If you want EIT data for quantitative research.... The following procedure should be followed to obtain the EIT data in FITS format: Determine which EIT data are available to support your study. An EIT team member can provide assistance throughout the whole process of obtaining data. To generate a list of available data, access the EIT WWW catalog interface or the Virtual Solar Observatory. The web catalog interface will provide a list and brief description of the data obtained over a range of dates. Keep in mind that the synoptic data and full-field images can also complement a study, so your data request needn't be restricted to a specific field of view or time cadence. Note that using the Web interface, you can now download compressed tar files of the EIT FITS files As a matter of courtesy, we ask that you send a preprint of any work involving EIT data to the EIT P.I., and after acceptance, a reprint to the EIT reprint library, care of Joe Gurman. EIT shutterless program The EIT group in the solar Physics Group at the Royal Observatory of Belgium is conducting a synoptic observing campaign using the high-cadence capability of the EIT instrument when run in shutterless readout mode. The latest running of the shutterless program results are available here. EIT Shutterless campaign, [Run #38] 2010 January 7 Seg 1 Preliminary Results 2010 January 7th 19:00 - 22:00 UT http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 3 of 9 EIT Shutterless campaign, [Run #38] 2010 January 14 Seg 2 Preliminary Results 2010 January 14th 19:00 - 22:30 UT For Archived Shutterless information, data, and movies; see The ROB High Cadence Pages EIT and Eclipses LASCO and EIT observing plan for 2001 June 21, including brief descriptions of the support requested by various eclipse expeditions The EIT Eclipse 2001 page, with images and useful links, will contain images from the days around (and of) the eclipse. The EIT Eclipse '99 page, with images and useful links, is now online. The EIT Eclipse '98 page, with images and useful links, is now online. EIT Calibration Rocket results The NRL/CSL/IAS EIT rocket flight to help calibrate the SOHO EIT was launched and recovered successfully on Thursday, 1997 October 16. Preliminary results indicate that, aside from a small light leak in the Fe XV 284 Å channel, the flight was fully successful. Exposure times and detector performance appear to have been nominal. Click on the thumbnail image on the left to access the NRL EIT calroc page. EIT Fe XII Å observations of disk coronal mass ejection and Moreton wave, 1999 July 19 Movies of a flare-related wave and dimming indicative of a possible earthward-directed coronal mass ejection (CME). http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 4 of 9 Difference GIF movie GIF movie 1999 July 19 00:00 - 03:36 UT EIT Fe XII Å observations of Solar Tornado, 1998 April 20 Movies of a helical field structure untwisting during a coronal mass ejection (CME). MPEG Movie QuickTime Movie Time 1998 April 20 08:11 - 11:02 UT Maps of the temperature-sensitive ratio (Fe XII 195 Å/ Fe IX, X 171 Å) The ratio is sensitive over the range 0.9 MK < Te < 1.5 MK. Ratio from Ratio from Ratio from Ratio from 1997 December 6 1997 December 7 1997 December 8 1997 December 9 07:00 - 07:12 UT 07:00 - 07:12 UT 07:00 - 07:12 UT 07:00 - 07:12 UT images images images images http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 5 of 9 Ratio from 1997 December 10 13:00 - 13:12 UT images Click on the thumbnail image for a full-resolution ratio map. Older EIT movies EIT movies from earlier observing sequences can be found on the new Cinema EIT page. OBE history A table showing when the OBE was loaded with new (or reloaded with older) software loads, and a partial listing of the new features introduced in those loads. EIT synoptic maps EIT synoptic maps in all four wavelengths in both GIF and FITS format are now available, courtesy of Elena Benevolenskaya at Stanford U. These include only central meridional charts. Additional EIT synoptic charts may be found at the NRL EIT/LASCO synoptic maps site EIT observing plan for tomorrow The SOHO observing plan for tomorrow includes EIT subfield target coordinates and areas, image times and wavelengths, and formal observing campaigns. EIT science topics At its 1996 March meeting, the EIT Consortium decided to list some initial research topics as well as volunteers from the consortium to lead the initial efforts in each area. These are not meant to be http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 6 of 9 exclusive or to indicate permanent rights of any sort, but it would benefit any prospective Guest Investigator (official or otherwise) to contact one of the Consortium members whose names are associated with a topic of interest to the Guest Investigator. The list can be thought of as the initial framework for the EIT Bulletin Board of proposed research. Go to the EIT science topics list. Current solar images from EIT The image on the left was obtained in the Fe XII emission line at 195 Å, while that on the right was obtained in He II 304 Å. Fe XII (eleven-times ionized Fe) is common at temperatures of 1.5 million K; He II is formed primarily at 60,000 - 80,000 K. The times at which these images were obtained are available on the SDAC "current solar images" page. While the pixel scale of the EIT instrument is 1024 x 1024 2.6-arc second pixels, the images to which these thumbnails are linked has been reduced to 512 x 512 to keep the file size reasonable (160 - 200 Kbyte). Full resolution GIF representations of EIT images can be found here. The LASCO/EIT observing program The two-month-long EIT and LASCO interim synoptic program, which began 1996 May 14, ended July 16 with the modification of the on-board software. The interim synoptic schedule decribes the former LASCO C1, C2, C3 and EIT "time slots" in the daily plan. The current observing schedule is much more flexible and varied, and can be obtained by checking either the SOHO daily targets page or the SOHO Daily Operations Database. What EIT is designed to do The SOHO EIT is able to image the solar transition region and inner corona in four, selected bandpasses in the extreme ultraviolet (EUV): Fe IX/X, 171 Å Fe XII, 195 Å Fe XV, 284 Å He II, 304 Å Using either full-disk or subfield images, the EIT can image active regions, filaments and prominences, coronal holes, coronal "bright points," polar plumes, and a variety of other solar features. The instrument was designed to be used in conjunction with other SOHO instruments, particularly the LASCO visible-light coronagraphs and the SUMER and CDS imaging spectrographs, as well as with ground-based instruments. http://umbra.nascom.nasa.gov/eit/ 4/9/2011 SOHO Extreme ultraviolet Imaging Telescope (EIT) Page 7 of 9 The instrument The EIT is a normal-incidence, multilayer telescope of novel design.
Load more

Recommended publications
  • Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares
    Space Sci Rev (2018) 214:45 https://doi.org/10.1007/s11214-018-0478-5 Modelling Quasi-Periodic Pulsations in Solar and Stellar Flares J.A. McLaughlin1 · V. M . N a k a r i a ko v 2,3,4 · M. Dominique5 · P. Jelínek6 · S. Takasao7 Received: 19 May 2017 / Accepted: 24 January 2018 / Published online: 6 February 2018 © The Author(s) 2018. This article is published with open access at Springerlink.com Abstract Solar flare emission is detected in all EM bands and variations in flux density of solar energetic particles. Often the EM radiation generated in solar and stellar flares shows a pronounced oscillatory pattern, with characteristic periods ranging from a fraction of a second to several minutes. These oscillations are referred to as quasi-periodic pulsa- tions (QPPs), to emphasise that they often contain apparent amplitude and period modu- lation. We review the current understanding of quasi-periodic pulsations in solar and stel- lar flares. In particular, we focus on the possible physical mechanisms, with an emphasis on the underlying physics that generates the resultant range of periodicities. These physi- cal mechanisms include MHD oscillations, self-oscillatory mechanisms, oscillatory recon- nection/reconnection reversal, wave-driven reconnection, two loop coalescence, MHD flow B J.A. McLaughlin [email protected] V.M. Nakariakov [email protected] M. Dominique [email protected] P. Jelínek [email protected] S. Takasao [email protected] 1 Northumbria University, Newcastle upon Tyne, NE1 8ST, UK 2 Centre for Fusion, Space and Astrophysics, University of Warwick, Coventry CV4 7AL, UK 3 School of Space Research, Kyung Hee University, Yongin, 446-701, Gyeonggi, Korea 4 St.
    [Show full text]
  • Estimate of Plasma Temperatures Across a CME-Driven Shock from a Comparison Between EUV and Radio Data
    Solar Phys (2020) 295:124 https://doi.org/10.1007/s11207-020-01686-0 Estimate of Plasma Temperatures Across a CME-Driven Shock from a Comparison Between EUV and Radio Data Federica Frassati1 · Salvatore Mancuso1 · Alessandro Bemporad1 Received: 9 March 2020 / Accepted: 6 August 2020 / Published online: 8 September 2020 © The Author(s) 2020 Abstract In this work, we analyze the evolution of an EUV wave front associated with a solar eruption that occurred on 30 October 2014, with the aim of investigating, through differential emission measure (DEM) analysis, the physical properties of the plasma com- pressed and heated by the accompanying shock wave. The EUV wave was observed by the Atmospheric Imaging Assembly (AIA) onboard the Solar Dynamics Observatory (SDO) and was accompanied by the detection of a metric Type II burst observed by ground-based radio spectrographs. The EUV signature of the shock wave was also detected in two of the AIA channels centered at 193 Å and 211 Å as an EUV intensity enhancement propagating ahead of the associated CME. The density compression ratio X of the shock as inferred from the analysis of the EUV data is X ≈ 1.23, in agreement with independent estimates obtained from the analysis of the Type II band-splitting of the radio data and inferred by adopting the upstream–downstream interpretation. By applying the Rankine–Hugoniot jump conditions under the hypothesis of a perpendicular shock, we also estimate the temperature ratio as TD/TU ≈ 1.55 and the post-shock temperature as TD ≈ 2.75 MK. The modest compression ratio and temperature jump derived from the EUV analysis at the shock passage are typical of weak coronal shocks.
    [Show full text]
  • Comprehensive Characterization of Solar Eruptions with Remote and In-Situ Observations, and Modeling: the Major Solar Events on 4 November 2015
    Solar Physics DOI: 10.1007/•••••-•••-•••-••••-• Comprehensive Characterization of Solar Eruptions With Remote and In-Situ Observations, and Modeling: The Major Solar Events on 4 November 2015 Iver H. Cairns?1 · Kamen A. Kozarev2 · Nariaki V. Nitta3 · Neus Agueda4 · Markus Battarbee5,6 · Eoin P. Carley7 · Nina Dresing8 · Ra´ulG´omez-Herrero9 · Karl-Ludwig Klein10 · David Lario11,12 · Jens Pomoell13 · Carolina Salas-Matamoros10,14 · Astrid M. Veronig15 · Bo Li1 · Patrick McCauley1 B Iver H. Cairns? [email protected],+61 2 9351 3961 Kamen A. Kozarev [email protected] Nariaki V. Nitta [email protected] Neus Agueda [email protected] Markus Battarbee [email protected] Eoin P. Carley [email protected] Nina Dresing [email protected] Ra´ulG´omez-Herrero [email protected] Karl-Ludwig Klein [email protected] David Lario [email protected] Jens Pomoell jens.pomoell@helsinki.fi Carolina Salas-Matamoros [email protected] Astrid M. Veronig arXiv:1910.03319v1 [astro-ph.SR] 8 Oct 2019 [email protected] Bo Li [email protected] SOLA: overview_51_8Oct19.tex; 9 October 2019; 0:35; p. 1 ISSI team: I.H. Cairns et al. c Springer •••• Abstract Solar energetic particles (SEPs) are an important product of solar activity. They are connected to solar active regions and flares, coronal mass ejections (CMEs), EUV waves, shocks, Type II and III radio emissions, and X- ray bursts. These phenomena are major probes of the partition of energy in solar eruptions, as well as for the organization, dynamics, and relaxation of coronal and interplanetary magnetic fields.
    [Show full text]
  • A Small-Scale Filament Eruption Inducing Moreton Wave, Euv Wave and Coronal Mass Ejection
    Draft version April 17, 2020 Preprint typeset using LATEX style AASTeX6 v. 1.0 A SMALL-SCALE FILAMENT ERUPTION INDUCING MORETON WAVE, EUV WAVE AND CORONAL MASS EJECTION Jincheng Wang1,2,3, Xiaoli Yan1,2, Defang Kong1,2, Zhike Xue1,2, Liheng Yang1,2, Qiaoling Li1,4 1Yunnan Observatories, Chinese Academy of Sciences, Kunming 650011, People.s Republic of China. 2Center for Astronomical Mega-Science, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing, 100012, People.s Republic of China 3CAS Key Laboratory of Solar Activity, National Astronomical Observatories, Beijing 100012, China 4University of Chinese Academy of Sciences, Yuquan Road, Shijingshan Block Beijing 100049, People.s Republic of China ABSTRACT With the launch of SDO, many EUV waves were observed during solar eruptions. However, the joint observations of Moreton and EUV waves are still relatively rare. We present an event that a small-scale filament eruption simultaneously results in a Moreton wave, an EUV wave and a Coronal Mass Ejection in active region NOAA 12740. Firstly, we find that some dark elongate lanes or fila- mentary structures in the photosphere existed under the small-scale filament and drifted downward, which manifests that the small-scale filament was emerging and lifting from subsurface. Secondly, combining the simultaneous observations in different Extreme UltraViolet (EUV) and Hα passbands, we study the kinematic characteristics of the Moreton and EUV waves. The comparable propagat- ing velocities and the similar morphology of Moreton and different passbands EUV wavefronts were obtained. We deduce that Moreton and different passbands EUV waves were the perturbations in dif- ferent temperature-associated layers induced by the coronal magneto-hydrodynamic shock wave.
    [Show full text]
  • Solar Activity and Its Evolution Across the Corona: Recent Advances
    J. Space Weather Space Clim. 3 (2013) A18 DOI: 10.1051/swsc/2013039 Ó F. Zuccarello et al., Published by EDP Sciences 2013 RESEARCH ARTICLE OPEN ACCESS Solar activity and its evolution across the corona: recent advances Francesca Zuccarello1,*, Laura Balmaceda2, Gael Cessateur3, Hebe Cremades4, Salvatore L. Guglielmino5, Jean Lilensten6, Thierry Dudok de Wit7, Matthieu Kretzschmar7, Fernando M. Lopez2, Marilena Mierla8,9,10, Susanna Parenti8, Jens Pomoell11, Paolo Romano5, Luciano Rodriguez8, Nandita Srivastava12, Rami Vainio11, Matt West8, and Francesco P. Zuccarello13 1 Dipartimento di Fisica e Astronomia, Sez. Astrofisica, Universita` di Catania, Via S. Sofia 78, 95123 Catania, Italy *Corresponding author: [email protected] 2 Instituto de Ciencias Astrono´micas, de la Tierra y el Espacio, ICATE-CONICET, Av. Espan˜a Sur 1512, J5402DSP, San Juan, Argentina 3 Physical-Meteorological Observatory/World Radiation Center, Davos, Switzerland 4 Universidad Tecnolo´gica Nacional – Facultad Regional Mendoza/CONICET, Rodrı´guez 273, M5502AJE, Mendoza, Argentina 5 INAF – Osservatorio Astrofisico di Catania, Via S. Sofia 78, 95123, Catania, Italy 6 UJF-Grenoble 1/CNRS-INSU, Institut de Plane´tologie et d’Astrophysique de Grenoble (IPAG) UMR 5274, 38041 Grenoble, France 7 LPC2E/CNRS (UMR 7328) and University of Orle´ans, 3A avenue de la Recherche Scientifique, 45071 Orle´ans Cedex 2, France 8 Solar – Terrestrial Center of Excellence – SIDC, Royal Observatory of Belgium, Av. Circulaire 3, 1180 Brussels, Belgium 9 Institute of Geodynamics
    [Show full text]
  • Absorption Phenomena and a Probable Blast Wave in the 13 July 2004 Eruptive Event
    Solar Physics DOI: 10.1007/•••••-•••-•••-••••-• Absorption Phenomena and a Probable Blast Wave in the 13 July 2004 Eruptive Event V.V. Grechnev1 · A.M. Uralov1 · V.A. Slemzin2 · I.M. Chertok3 · I.V. Kuzmenko4 · K. Shibasaki5 Received ; accepted c Springer •••• Abstract We present a case study of the 13 July 2004 solar event, in which disturbances caused by eruption of a filament from an active region embraced a quarter of the visible solar surface. Remarkable are absorption phenomena observed in the SOHO/EIT 304 A˚ channel; they were also visible in the EIT 195 A˚ channel, in the Hα line, and even in total radio flux records. Coronal and Moreton waves were also observed. Multi-spectral data allowed reconstructing an overall picture of the event. An explosive filament eruption and related impulsive flare produced a CME and blast shock, both of which decelerated and propagated independently. Coronal and Moreton waves were kinematically close and both decelerated in accordance with an expected motion of the coronal blast shock. The CME did not resemble a classical three-component structure, probably, because some part of the ejected mass fell back onto the Sun. Quantitative evaluations from different observations provide close estimates of the falling mass, ∼ 3 · 1015 g, which is close to the estimated mass of the CME. The falling material was responsible for the observed large-scale absorption phenomena, in particular, shallow widespread moving dimmings observed at 195 A.˚ By contrast, deep quasi-stationary dimmings observed in this band near the eruption center were due to plasma density decrease in coronal structures.
    [Show full text]
  • A Unified View of Solar Flares and Coronal Mass Ejections
    2001.6.18 at Longmont, Colorado A Unified View of Solar Flares and Coronal Mass Ejections K. Shibata Kyoto University, Kwasan Observatory Contents 1. Introduction 2. Recent Space Observations of Solar Flares and Coronal Mass Ejections - Yohkoh, SOHO, TRACE increasing evidence of magnetic reconnection and plasmoid ejections 3. A Unified Model of Solar Flares/CMEs - plasmoid-induced-reconnection model - Numerical Simulations 4. Summary and Remaining Questions 1. Introduction Solar flares H alpha discovered by Carrington and Hodgson (~1860) Energy source = Magnetic energy Size ～109 –1010 cm Total energy 1029 –1032 erg Ｈα (Kyoto/Hida) Electro- magnetic waves emitted from solar flares (Svestka 1976) Solar flares are often associated with prominence eruptions （１９４５年６月２８日、HAO) Reconnection model (CSHKP model=Carmichael 1964, Sturrock 1966, Hirayama 1974, Kopp-Pneuman 1976) Basic puzzles of solar flares before Yohkoh (1991) • Reconnection theory has not yet been established • Many authorities doubted reconnection model (e.g., Alfven, Akasofu, Uchida, Melrose, ….) current disruption vs reconnection • There are many flares which are NOT associated with prominence eruptions • There was no direct observational evidence of reconnection in flares Coronal Mass Ejections (CMEs) • discovered in 1970s with space coronagraph • cause geomagnetic storm • many CMEs are not associated with flares, but with filament eruptions Basic questions about coronal mass ejections (CMEs) • Are CMEs more important than flares ? (Gosling 1993) • What is the relation between CMEs and flares ? Are CMEs different from flares ? • Is reconnection important in CMEs ? 2. Recent Space Observations of Solar Flares and CMEs • Yohkoh (陽光) Aug. 30, 1991 ー present • Japan-US-UK collaboration • soft X-ray telescope (SXT~1keV) hard X-ray telescope (HXT~10-100keV) Solar corona observed with soft X-ray telescope (SXT) aboard Yohkoh Soft X-ray （～1 keV) 2MK－20MK Note numerous microflares 2D view of reconnection (CSHKP) model ⇒should be observed in Soft-Xrays LDE (long duration event) flare (SXT, ～１keV、 Tsuneta et al.
    [Show full text]
  • Solar Type II Radio Bursts Associated with CME Expansions As Shown by EUV Waves
    A&A 578, A38 (2015) Astronomy DOI: 10.1051/0004-6361/201425388 & c ESO 2015 Astrophysics Solar type II radio bursts associated with CME expansions as shown by EUV waves R. D. Cunha-Silva, F. C. R. Fernandes, and C. L. Selhorst IP&D – Universidade do Vale do Paraíba – UNIVAP, Av. Shishima Hifumi, 2911 Urbanova, São José dos Campos, SP, Brazil e-mail: [email protected] Received 21 November 2014 / Accepted 9 April 2015 ABSTRACT Aims. We investigate the physical conditions of the sources of two metric type II bursts associated with coronal mass ejection (CME) expansions with the aim of verifying the relationship between the shocks and the CMEs by comparing the heights of the radio sources and of the extreme-ultraviolet (EUV) waves associated with the CMEs. Methods. The heights of the EUV waves associated with the events were determined in relation to the wave fronts. The heights of the shocks were estimated by applying two different density models to the frequencies of the type II emissions and compared with the heights of the EUV waves. For the event on 13 June 2010 that included band-splitting, the shock speed was estimated from the frequency drifts of the upper and lower frequency branches of the harmonic lane, taking into account the H/F frequency ratio fH/ fF = 2. Exponential fits on the intensity maxima of the frequency branches were more consistent with the morphology of the spectrum of this event. For the event on 6 June 2012 that did not include band-splitting and showed a clear fundamental lane on the spectrum, the shock speed was directly estimated from the frequency drift of the fundamental emission, determined by linear fit on the intensity maxima of the lane.
    [Show full text]
  • Moreton Waves Related to the Solar Eruption
    Publications of the Korean Astronomical Society pISSN: 1225-1534 30: 057 ∼ 058, 2015 September eISSN: 2287-6936 ⃝c 2015. The Korean Astronomical Society. All rights reserved. http://dx.doi.org/10.5303/PKAS.2015.30.2.057 MORETON WAVES RELATED TO THE SOLAR ERUPTION OCCURRED ON 3 JUNE 2012 AND 6 JULY 2012 Agustinus Gunawan admiranto1 & Rhorom Priyatikanto1,2 1National Institute of Aeronautics and Space, Indonesia 2Astronomy Program, Institut Teknologi Bandung, Indonesia E-mail: gun [email protected] & [email protected] (Received November 30, 2014; Reviced May 31, 2015; Aaccepted June 30, 2015) ABSTRACT In this study, we present geometrical and kinematical analysis of Moreton wave observed in 2012 June 3rd and July 6th, recorded in H-α images of Global Oscillation Network Group (GONG) archive. These large-scale waves exhibit different features compared to each other. The observed wave of June 3rd has angular span of about 70◦ with a diffuse wave front associated to NOAA active region 11496. It was found that the propagating speed of the wave at 17:53 UT is about 931 80 km/s. The broadness nature of this Moreton wave can be interpreted as the vertical extension of the wave over the chromosphere. On the other hand, the wave of July 6th associated with X1.1 class flare that occurred at 23:01 UT in AR NOAA11515. From the kinematical analysis, the wave propagated with the initial velocity of about 994 70 km/s which is in agreement with the speed of coronal shock derived from type II radio burst, v ∼ 1100 km/s.
    [Show full text]
  • The Sun and Heliosphere in Three Dimensions
    The Sun and Heliosphere In Three Dimensions Report of the NASA Science Definition Team for the STEREO Mission Table of Contents Executive Summary ........................................................................................................... 1 1. Introduction ..................................................................................................................3 2. Scientific Objectives ..................................................................................................... 4 Coronal Mass Ejections ....................................................................................................................... 4 CME Onset ..................................................................................................................................... 4 CME Geometry and Onset Signatures............................................................................................ 5 Reconnection .................................................................................................................................. 6 Surface Evolution ........................................................................................................................... 6 The Heliosphere Between the Sun and Earth ...................................................................................... 7 CMEs in the Heliosphere ..................................................................................................................... 9 Tracking Disturbances from the Sun to Earth ..................................................................................
    [Show full text]
  • Magnetohydrodynamic Oscillations in the Solar Corona and Earth’S Magnetosphere: Towards Consolidated Understanding
    Noname manuscript No. (will be inserted by the editor) Magnetohydrodynamic Oscillations in the Solar Corona and Earth's Magnetosphere: Towards Consolidated Understanding V. M. Nakariakov · V. Pilipenko · B. Heilig · P. Jel´ınek · M. Karlick´y · D.Y. Klimushkin · D.Y. Kolotkov · D.-H. Lee · G. Nistic`o · T. Van Doorsselaere · G. Verth · I.V. Zimovets Received: date / Accepted: date V. M. Nakariakov Centre for Fusion, Space and Astrophysics, University of Warwick, Coventry CV4 7AL, UK, School of Space Research, Kyung Hee University, Yongin, 446-701, Gyeonggi, Korea, Central Astronomical Observatory at Pulkovo, St Petersburg 196140, Russia, E-mail: [email protected] V.A. Pilipenko Space Research Institute, Moscow 117997, Russia B. Heilig Tihany Geophysical Observatory, Geological and Geophysical Institute of Hungary, Tihany, Hungary P. Jel´ınek Institute of Physics and Biophysics, Faculty of Science, University of South Bohemia, CZ - 370 05 Cesk´eBudˇejovice,ˇ Czech Republic M. Karlick´y Astronomical Institute of the Academy of Sciences of the Czech Republic, 25165, Ondˇrejov, Czech Republic D.Y. Klimushkin Institute of Solar-Terrestrial Physics, Lermontov St. 126A, Irkutsk 664033, Russia D.Y. Kolotkov Centre for Fusion, Space and Astrophysics, University of Warwick, Coventry CV4 7AL, UK, D.-H. Lee School of Space Research, Kyung Hee University, Yongin, 446-701, Gyeonggi, Korea G. Nistic`o Centre for Fusion, Space and Astrophysics, University of Warwick, Coventry CV4 7AL, UK T. Van Doorsselaere Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, B- 3001 Leuven, Belgium G. Verth Solar Physics and Space Plasma Research Centre (SP2RC), University of Sheffield, Sheffield S3 7RH, UK I.V.
    [Show full text]
  • Seismology of the Corona of The
    Coronal seismology n Sunday 1 November 1755 a strong earthquake accompanied by a tsunami Odevastated the city of Lisbon and left 70 000 inhabitants dead. This dramatic event Seismology of the triggered a new approach in understanding the forces of the Earth: seismology. In more general terms, seismology is the remote diagnostics of media by means of waves. Seismology has corona of the Sun become a well-developed technique in various applications; as well as seismology of the Earth’s interior, there are ultrasound scans of V M Nakariakov and E Verwichte put seismology to work in the study the human body and marine acoustics (sonars), of the solar corona, the hot atmosphere of the Sun. and a less familiar but important application in laboratory plasma spectroscopy. The first Abstract implementation of this technique in solar flare epicentre physics – helioseismology – is connected with Seismology now includes study of the kink oscillations solar surface oscillations, discovered by Robert Sun’s corona, a promising research target loop Leighton in the early 1960s. These oscillations both in its own right and for its role in were interpreted in terms of acoustic-gravita- the relationship between the Sun and the tional waves and now provide unique informa- Earth and its links to the solar magnetic tion about the solar interior, its structure and blast wave footpoint field. In addition, the corona, as a natural (fast magnetoacoustic) differential rotation – and even about the far plasma, is itself an objective for footpoint side of the Sun (see discussion by Thompson, fundamental physics. Observations using this issue p4.21–4.25).
    [Show full text]