Polarization Measurements at the Daniel K. Inouye Solar Telescope (formerly ATST) Valentin Martinez Pillet David Elmore
|
|
- Rolf Collins
- 6 years ago
- Views:
Transcription
1 Polarization Measurements at the Daniel K. Inouye Solar Telescope (formerly ATST) Valentin Martinez Pillet David Elmore
2 Summary Inouye Solar Telescope will observationally test models with spatial resolution 2.5X any existing solar telescope Science cases in the Critical Science Plan require spectropolarimetry Suite of spectro-polarimeters with wavelengths spanning μm μm μm μm Multiple S-Ps operate simultaneously each sensing multiple pass bands permitting multi-line diagnostics B vector vs. height, separate temperature from velocity, fill factor,
3 Overview of Observatory 10/26/2014 3
4 SPIE Montreal 4
5 East-West Section Through Site (work Oct 2014 shown in color) Pre-Cast Siding Platform Lift Assy Also completed but not shown: 1) site infrastructure & electrical transformers; 2) backfeed electrical, comm., and fiber to IfA facilities; 3) retaining wall & roadwork 10/26/2014 5
6 Enclosure 10/26/2014 6
7 Telescope Mount Assembly Alt-Az Mount 10/26/2014 Coudé Rotator 7
8
9
10
11 DKIST Technical Specifications: 4 m aperture, off-axis Gregorian Integrated adaptive optics. Hybrid enclosure with thermal control and dust mitigation. Field of view: 5 arcminutes. Angular resolution < μ Polarization accuracy 0.05%. Wavelength range microns, microns at commissioning. Coronagraphic capabilities in IR Facility instruments: VBI: nm VISP: nm VTF: nm Cryo-NIRSP: nm DL-NIRSP: nm 11
12 DKIST CRITICAL SCIENCE PLAN (CSP) DKIST CSP outlines the specific science topics that the telescope will address in the first 1-2 years of commissioning/operations. Goal is to develop detailed observing proposals (next slide) to address specific science questions. This will help to - facilitate early science - clarify operations and pipeline data processing needs - instrument validation DKIST CSP: Community driven with discussion led by the DKIST Science Working Group Chair (Mark Rast) Described in a living document that will be updated as needed. Specro-polarimetry is critical to nearly CSP science topics
13 Magnetoconvection physics Formation of kilogauss fields in the photosphere (Knölker) Structure & dynamics of small-scale magnetic elements (Criscuoli,Cauzzi) Magnetic field transport: surface dynamo phenomena (Rast) Sunspot umbral structure (Balasubramaniam) Sunspot penumbral formation and structure (Tritschler, TBD) Wave generation and propagation local helioseismology (TBD)
14 Dynamo processes and magnetohydrodynamics: Small-scale photospheric magnetic fields: formation, structure, dynamics (Brown) Turbulent dynamo: Hanle effect imaging of the quiet-sun (Bellot) Wave generation and propagation (Rast) Magnetoconvective modulation of solar luminosity (Criscuoli) Sunspots: umbral and penumbral structure and dynamics (Tritschler) Flux emergence and active region formation (Katsukawa) Magnetic connectivity and energy flows in the outer atmosphere: The chromosphere/corona connection (Cao) Spicule physics (McIntosh) Formation, evolution, and eruption of non-potential configurations (Parnell) Multilayer magnetometry and atmospheric heating (Socas-Navarro) Coronal waves and energy fluxes (Cranmer) Energy and magnetic helicity in coronal structures (Judge) Prominence morphology, connectivity, and life cycles (Scullion) Infra-red survey of the solar atmosphere (Penn) Flares and eruptive activity: Flare precursors in the lower atmosphere Magnetic field connectivity and changes in flares (Qiu) Flare electron diagnostics in visible light (Cauzzi) Flare foot points at their fundamental scales (Fletcher) CMEs Miscellaneous topics: Sun-grazing comets (Liu) Under revision!!
15 Magnetic connectivity and energy flows in the outer atmosphere The chromosphere/corona connection (Judge) Spicule physics (Cao, Carlsson) Coronal imaging (Woger, TBD) Coronal magnetometry (Judge) Quiet-Sun magnetic activity (DeForest, Deng)
16 Dynamo processes and magnetohydrodynamics: Small-scale photospheric magnetic fields: formation, structure, dynamics (Brown) Turbulent dynamo: Hanle effect imaging of the quiet-sun (Bellot) Wave generation and propagation (Rast) Magnetoconvective modulation of solar luminosity (Criscuoli) Sunspots: umbral and penumbral structure and dynamics (Tritschler) Flux emergence and active region formation (Katsukawa) Magnetic connectivity and energy flows in the outer atmosphere: The chromosphere/corona connection (Cao) Spicule physics (McIntosh) Formation, evolution, and eruption of non-potential configurations (Parnell) Multilayer magnetometry and atmospheric heating (Socas-Navarro) Coronal waves and energy fluxes (Cranmer) Energy and magnetic helicity in coronal structures (Judge) Prominence morphology, connectivity, and life cycles (Scullion) Infra-red survey of the solar atmosphere (Penn) Flares and eruptive activity: Flare precursors in the lower atmosphere Magnetic field connectivity and changes in flares (Qiu) Flare electron diagnostics in visible light (Cauzzi) Flare foot points at their fundamental scales (Fletcher) CMEs Miscellaneous topics: Sun-grazing comets (Liu) Under revision!!
17 Flares and eruptive activity Formation and evolution of prominences and coronal cavity systems (Berger, Gibson) Flare precursors in the lower atmosphere (TBD) Flare footpoint dynamics (Fletcher, Qiu) Flare electron diagnostics in visible light (Fletcher, Cauzzi)
18 Dynamo processes and magnetohydrodynamics: Small-scale photospheric magnetic fields: formation, structure, dynamics (Brown) Turbulent dynamo: Hanle effect imaging of the quiet-sun (Bellot) Wave generation and propagation (Rast) Magnetoconvective modulation of solar luminosity (Criscuoli) Sunspots: umbral and penumbral structure and dynamics (Tritschler) Flux emergence and active region formation (Katsukawa) Magnetic connectivity and energy flows in the outer atmosphere: The chromosphere/corona connection (Cao) Spicule physics (McIntosh) Formation, evolution, and eruption of non-potential configurations (Parnell) Multilayer magnetometry and atmospheric heating (Socas-Navarro) Coronal waves and energy fluxes (Cranmer) Energy and magnetic helicity in coronal structures (Judge) Prominence morphology, connectivity, and life cycles (Scullion) Infra-red survey of the solar atmosphere (Penn) Flares and eruptive activity: Flare precursors in the lower atmosphere Magnetic field connectivity and changes in flares (Qiu) Flare electron diagnostics in visible light (Cauzzi) Flare foot points at their fundamental scales (Fletcher) CMEs Miscellaneous topics: Sun-grazing comets (Liu) Under revision!!
19 Miscellaneous topics Sun-grazing comets (Liu, Wooden, Berger) Infra-Red survey of the solar atmosphere (Penn, Judge, Ayres) High-resolution Hanle Effect survey (Martinez-Pillet, Judge)
20 Dynamo processes and magnetohydrodynamics: Small-scale photospheric magnetic fields: formation, structure, dynamics (Brown) Turbulent dynamo: Hanle effect imaging of the quiet-sun (Bellot) Wave generation and propagation (Rast) Magnetoconvective modulation of solar luminosity (Criscuoli) Sunspots: umbral and penumbral structure and dynamics (Tritschler) Flux emergence and active region formation (Katsukawa) Magnetic connectivity and energy flows in the outer atmosphere: The chromosphere/corona connection (Cao) Spicule physics (McIntosh) Formation, evolution, and eruption of non-potential configurations (Parnell) Multilayer magnetometry and atmospheric heating (Socas-Navarro) Coronal waves and energy fluxes (Cranmer) Energy and magnetic helicity in coronal structures (Judge) Prominence morphology, connectivity, and life cycles (Scullion) Infra-red survey of the solar atmosphere (Penn) Flares and eruptive activity: Flare precursors in the lower atmosphere Magnetic field connectivity and changes in flares (Qiu) Flare electron diagnostics in visible light (Cauzzi) Flare foot points at their fundamental scales (Fletcher) CMEs Miscellaneous topics: Sun-grazing comets (Liu) Under revision!!
21 . Making an unambiguous connection between model results and observations requires the forward modeling of spectral lines and detailed comparison with observations,... (Rempel & Schlichenmaier LRSP) Courtesy M. Rempel Courtesy F. Wöger D=0.75m D=1.5m D=4m Model Putting models to the test: Resolution, resolution, resolution
22 Photospheric field: FeI 525nm, FeI 630.2nm, FeI 1.56μm lines Chromospheric field: CaII 854.2nm, HeI nm Coronal field: FeXIII μm, SiIX 3.9μm 3D structure of magnetic field diagnostic tools: UV far IR coverage Credit: B. DePontieu Credit: NASA/ESA/LMSAL. Field extrapolation
23 The coronal magnetic field controls the plasma dynamics. The magnetic field: Can be modeled using extrapolations Has been estimated with proxies Measurements are mostly lacking!
24 Courtesy J. Kuhn
25 Bak-Steslicka et al (2013) measure the magnetic morphology of prominence cavities using HAO COMP data The technique uses linear polarization of Fe XIII 1075nm and forward modeling.
26 Spectrograph Inversion-driven physics requiring instantaneous realization of the Stokes profiles. Multiple line diagnostics within spectral band Wavelength Y Tunable Filtergraph Spatial correlation of widely-separated features is required. Image reconstruction techniques over a wide field. Imaging Spectrograph Strict simultaneity of both spectral and spatial samples is required. 26
27 Cryogenic Near Infrared Spectro- Polarimeter (Cryo-NIRSP)
28 Cryogenic Near Infrared Spectro- Polarimeter (Cryo-NIRSP) Jeff Kuhn IfA University of Hawaii Cryogenic spectrograph and imager with pass bands between 1.0μm and 5.0μm Full Stokes spectro-polarimetry 180x240 arcsecond 2 scanned field of view Coronal lines 1.075μm, 1.080μm, 3.95μm. CO at 4.66μm
29 Visible Spectro-Polarimeter (ViSP)
30 Visible Spectro-Polarimeter (ViSP) Roberto Casini High Altitude Observatory From 30 lines of interest between 380nm and 1100nm: probability of observing 1 line = 100% 2 lines = 98% 3 lines = 85% Broad spectral bands for even more lines that can be simultaneously observed
31 Visible Tunable Filter (VTF)
32 Visible Tunable Filter (VTF) Wolfgang Schmidt KIS Freiburg Scanning Fabry-Perot spectro-polarimeter Selected lines between 520nm and 870nm Image reconstruction over 1 arcmin 2 field of view.
33 Diffraction Limited Near Infrared Spectro-polarimeter (DL-NIRSP)
34 Diffraction Limited Near Infrared Spectro-polarimeter (DL-NIRSP) Haosheng Lin IfA University of Hawaii Imaging spectro-polarimeter Three channels. DWDM filters within 500nm 900nm 900nm 1350nm 1350nm 1800nm+ Spatial sample sizes of 0.03, 0.08, and 0.42 arc seconds 2 Fields of view of 1.8x2.4, 3.6x4.8, and 20x30 arc seconds 2
35 Summary Inouye Solar Telescope will observationally test models with spatial resolution 2.5X any existing solar telescope Science cases in the Critical Science Plan require spectropolarimetry Suite of spectro-polarimeters with wavelengths spanning μm μm μm μm Multiple S-Ps operate simultaneously each sensing multiple pass bands permitting multi-line diagnostics B vector vs. height, separate temperature from velocity, fill factor,
36 36
Visible Spectro-Polarimeter (ViSP) Instrument Science Requirement
Project Documentation Document SPEC-0055 Revision D Visible Spectro-Polarimeter (ViSP) Instrument Science Requirement D. Elmore 1, H. Socas-Navarro, R. Casini 3 June 2014 Released By: Name Joseph McMullin
More informationPolarimetry Working Group Recommendations on Telescope Calibration and Polarization Modulator Location
Project Documentation Document RPT-0046 Draft A3 Polarimetry Working Group Recommendations on Telescope Calibration and Polarization Modulator Location David Elmore ATST Instrument Scientist 1 November
More informationA down-to-earth guide to high-resolution solar observations. Kevin Reardon National Solar Observatory
A down-to-earth guide to high-resolution solar observations Kevin Reardon kreardon@nso.edu National Solar Observatory Seeing Adaptive Optics Image Reconstruction Atmospheric Effects Spectral Lines Calibration
More informationEnd-to-end simulations of the Visible Tunable Filter for the Daniel K. Inouye Solar Telescope
End-to-end simulations of the Visible Tunable Filter for the Daniel K. Inouye Solar Telescope Wolfgang Schmidt, Matthias Schubert, Monika Ellwarth, Jörg Baumgartner, Alexander Bell, Andreas Fischer, Clemens
More informationCryogenic Near-IR Spectro-Polarimeter (Cryo-NIRSP) Instrument Science Requirement Document
Project Documentation Document SPEC-0056 Revision D Cryogenic Near-IR Spectro-Polarimeter (Cryo-NIRSP) Instrument Science Requirement Document M. Penn, J. Kuhn, D. Elmore * Instrument Group 28 July 2010
More informationCoronal Magnetometry Jean Arnaud, Marianne Faurobert, Gérad Grec et Jean-Claude Vial. Jean Arnaud Marianne Faurobert Gérard Grec et Jean-Claude Vial
Coronal Magnetometry Jean Arnaud, Marianne Faurobert, Gérad Grec et Jean-Claude Vial Jean Arnaud Marianne Faurobert Gérard Grec et Jean-Claude Vial INTRODUCTION The solar corona is a high temperature and
More informationCommon questions when planning observations with DKIST Jan 30, 2018
Common questions when planning observations with DKIST Jan 30, 2018 1. Can the DKIST instruments work together? All instruments except Cryo-NIRSP can work together and with Adaptive Optics (AO). All can
More informationpre Proposal in response to the 2010 call for a medium-size mission opportunity in ESA s science programme for a launch in 2022.
Solar magnetism explorer (SolmeX) Exploring the magnetic field in the upper atmosphere of our closest star preprint at arxiv 1108.5304 (Exp.Astron.) or search for solmex in ADS Hardi Peter & SolmeX team
More informationCoronal magnetometry
Coronal magnetometry status report February 13, 2006 Philip Judge & Steven Tomczyk High Altitude Observatory, NCAR, Boulder CO, USA Coronal magnetometry p.1/21 The challenge we wish to measure coronal
More informationThe Solar Physics Research Integrated Network Group SPRING
The Solar Physics Research Integrated Network Group Markus Roth, Sanjay Gosain, Frank Hill, Michael Thompson European Space Weather Week November 23, 2015 The Need for Synoptic Observations of the Sun
More informationATST Science Requirements Document
Project Documentation Specification #0001 Revision B ATST Science Requirements Document Thomas Rimmele Science Team December 12, 2005 Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ
More informationarxiv: v1 [astro-ph.sr] 13 Nov 2015
Polarimetry: From the Sun to Stars and Stellar Environments Proceedings IAU Symposium No. 305, 2015 K. N. Nagendra, S. Bagnulo, c 2015 International Astronomical Union R. Centeno & M.J. Martinez Gonzalez,
More informationThe Sun s Dynamic Atmosphere
Lecture 16 The Sun s Dynamic Atmosphere Jiong Qiu, MSU Physics Department Guiding Questions 1. What is the temperature and density structure of the Sun s atmosphere? Does the atmosphere cool off farther
More informationIntroduction to the Chinese Giant Solar Telescope
First Asia-Pacific Solar Physics Meeting ASI Conference Series, 2011, Vol. 2, pp 31 36 Edited by Arnab Rai Choudhuri & Dipankar Banerjee Introduction to the Chinese Giant Solar Telescope Y. Y. Deng (On
More informationSolar-B. Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University
Solar-B Report from Kyoto 8-11 Nov Meeting organized by K. Shibata Kwasan and Hida Observatories of Kyoto University The mission overview Japanese mission as a follow-on to Yohkoh. Collaboration with USA
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 2 12 Jun 07 UA/NSO Summer School 1 Solar Magnetic Fields 2 (12 June) An introduction to the instruments and techniques used to remotely measure the solar magnetic field Stokes Vectors
More informationMcMath-Pierce Adaptive Optics Overview. Christoph Keller National Solar Observatory, Tucson
McMath-Pierce Adaptive Optics Overview Christoph Keller National Solar Observatory, Tucson Small-Scale Structures on the Sun 1 arcsec Important astrophysical scales (pressure scale height in photosphere,
More informationCOSMO. The COronal Solar Magnetism Observatory
COSMO The COronal Solar Magnetism Observatory A Response to the Request for Information from the NRC Decadal Survey in Solar and Space Physics Steven Tomczyk 1*, Joan Burkepile 1, Roberto Casini 1, Giuliana
More informationMeasuring the Magnetic Vector with the Hei Å Line: A Rich New World
Solar Polarization 4 ASP Conference Series, Vol. 358, 2006 R. Casini and B. W. Lites Measuring the Magnetic Vector with the Hei 10830 Å Line: A Rich New World S. K. Solanki, 1 A. Lagg, 1 R. Aznar Cuadrado,
More informationNear Infrared Spectro-Polarimeter Use Case
Project Documentation RPT-0036 Revision A Near Infrared Spectro-Polarimeter Use Case S. Gibson, L. Fletcher, R. Hubbard, S. Keil, J. Kuhn, H. Lin, M. Penn Science Working Group May 2008 Approved for use:
More informationVisible Spectro-Polarimeter Use Case
Project Documentation RPT-0032 Revision A Visible Spectro-Polarimeter Use Case Alexandra Tritschler, David Elmore, Craig DeForest, Peter Nelson, Rebecca Centeno-Elliot Science Working Group May 2008 Approved
More informationProposed National Large Solar Telescope. Jagdev Singh Indian Institute of Astrophysics, Bangalore , India.
J. Astrophys. Astr. (2008) 29, 345 351 Proposed National Large Solar Telescope Jagdev Singh Indian Institute of Astrophysics, Bangalore 560 034, India. e-mail: jsingh@iiap.res.in Abstract. Sun s atmosphere
More informationA Large Coronagraph for Solar Coronal Magnetic Field Measurements
A Large Coronagraph for Solar Coronal Magnetic Field Measurements Steven Tomczyk HAO, NCAR High Altitude Observatory (HAO) National Center for Atmospheric Research (NCAR) The National Center for Atmospheric
More informationMulti-Application Solar Telescope Preliminary results
Preliminary results Shibu K. Mathew Udaipur Solar Observatory Past Present Future Telescope specs. and components Installation Optical alignment and tests Back-end instruments Preliminary observations
More informationVector Magnetic Field Diagnostics using Hanle Effect
Meeting on Science with Planned and Upcoming Solar Facilities in the Country, Bangalore, India, November 2-3, 2011 Vector Magnetic Field Diagnostics using Hanle Effect M. Sampoorna Indian Institute of
More informationOn the nature of Ellermanbombs and microflaresas observed with the 1.5m GREGOR telescope
On the nature of Ellermanbombs and microflaresas observed with the 1.5m GREGOR telescope C. Kuckein 1, N. Bello González 2, C. Denker 1, P. Gömöry 3, H. Strecker 2, R. Schlichenmaier 2 and the GFPI 1 &
More informationFIRS: A New Instrument for Multi-Wavelength Spectropolarimetry
: A New Instrument for Multi-Wavelength Spectropolarimetry Sarah Jaeggli, Haosheng Lin Institute for Astronomy, University of Hawai i is supported by the National Science Foundation Major Research Program,
More informationSolar Astrophysics with ALMA. Sujin Kim KASI/EA-ARC
Solar Astrophysics with ALMA Sujin Kim KASI/EA-ARC Contents 1. The Sun 2. ALMA science targets 3. ALMA capabilities for solar observation 4. Recent science results with ALMA 5. Summary 2 1. The Sun Dynamic
More informationAdvanced Technology Solar Telescope Design and Development Phase
Advanced Technology Solar Telescope Design and Development Phase Appendix I. SCIENCE Proposal to the National Science Foundation Submitted by Association of Universities for Research in Astronomy, Inc.
More informationPhotospheric magnetism
Photospheric magnetism SAMI K. SOLANKI MAX PLANCK INSTITUTE FOR SOLAR SYSTEM RESEARCH Large and small magnetic features Polar fields 2 4 10 26 Mx/yr Quiet network Internetwork fields 10 28 Mx/yr Active
More informationNST Instrumentation and Data. Big Bear Solar Observatory
NST Instrumentation and Data 1.6 m Clear Aperture Off-Axis Telescope New Solar Telescope The New Solar Telescope Optical Configuration The NST configuration is a 1/5 scale copy of one segment of the
More informationSolar Optical Telescope onboard HINODE for Diagnosing the Solar Magnetic Fields
Solar Optical Telescope onboard HINODE for Diagnosing the Solar Magnetic Fields Kiyoshi Ichimoto 1) and HINODE/SOT-team 1) Solar-B Project Office National Astronomical Observatory /NINS 16 th International
More informationMolecule Formation and Magnetic Field Evolution in Sunspots
**Volume Title** ASP Conference Series, Vol. **Volume Number** **Author** c **Copyright Year** Astronomical Society of the Pacific Molecule Formation and Magnetic Field Evolution in Sunspots S. A. Jaeggli
More informationThe Uncombed Penumbra
Solar Polarization 4 ASP Conference Series, Vol. 358, 2006 R. Casini and B. W. Lites The Uncombed Penumbra J. M. Borrero and M. Rempel High Altitude Observatory, National Center for Atmospheric Research,
More informationSolar Magnetic Fields Jun 07 UA/NSO Summer School 1
Solar Magnetic Fields 1 11 Jun 07 UA/NSO Summer School 1 If the sun didn't have a magnetic field, then it would be as boring a star as most astronomers think it is. -- Robert Leighton 11 Jun 07 UA/NSO
More informationC PROJECT DESCRIPTION C.1 Overview
C PROJECT DESCRIPTION C.1 Overview Understanding the Sun has always been a vital quest of science because the Sun is the most significant astronomical object for humankind. Exciting observations of solar
More informationIntroduction to Daytime Astronomical Polarimetry
Introduction to Daytime Astronomical Polarimetry Sami K. Solanki Max Planck Institute for Solar System Research Introduction to Solar Polarimetry Sami K. Solanki Max Planck Institute for Solar System Research
More informationObservational programs at Istituto Ricerche Solari Locarno (IRSOL)
Observational programs at Istituto Ricerche Solari Locarno (IRSOL) Renzo Ramelli and IRSOL collaborators IRSOL Locarno, Switzerland Suzhou, China 24th July 2009 Scientific Collaborators affiliated to IRSOL
More informationThe Solar-C; Current status
The Solar-C; Current status Kiyoshi Ichimoto (Kyoto Univ./NAOJ) and SOLAR-C Working Group Sac Peak Workshop, 2017.8.7-11; High-resolution solar physics: past, present, future Many Hinode results are related
More informationThe Interior Structure of the Sun
The Interior Structure of the Sun Data for one of many model calculations of the Sun center Temperature 1.57 10 7 K Pressure 2.34 10 16 N m -2 Density 1.53 10 5 kg m -3 Hydrogen 0.3397 Helium 0.6405 The
More informationOutline. Astronomy: The Big Picture. Earth Sun comparison. Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned.
Nighttime observing is over, but a makeup observing session may be scheduled. Stay tuned. Next homework due Oct 24 th. I will not be here on Wednesday, but Paul Ricker will present the lecture! My Tuesday
More informationUV spectro-polarimetry with CLASP & CLASP2 sounding rocket experiments
UV spectro-polarimetry with CLASP & CLASP2 sounding rocket experiments R. Ishikawa (1), R. Kano (1), A. Winebarger (2), D. E. McKenzie (2), F. Auchere (3), J. Trujillo Bueno (4), N. Narukage (1), K. Kobayashi
More informationPolarization Calibration Plan
Project Documentation Document RPT-0055 Revision A Polarization Calibration Plan David Elmore Science Team 3 September 2015 Advanced Technology Solar Telescope 950 N. Cherry Avenue Tucson, AZ 85719 Phone
More informationINFERENCE OF CHROMOSPHERIC MAGNETIC FIELDS IN A SUNSPOT DERIVED FROM SPECTROPOLARIMETRY OF Ca II 8542 A
Al-Azhar Bull. Sci. INFERENCE OF CHROMOSPHERIC MAGNETIC FIELDS IN A SUNSPOT DERIVED FROM SPECTROPOLARIMETRY OF Ca II 8542 A Ali G. A. Abdelkawy 1, Abdelrazek M. K. Shaltout 1, M. M. Beheary 1, T. A. Schad
More informationSolar InfraRed COronal Magnetograph (SIRCOM) Proposal for a space based coronagraph for vector magnetic field measurements
Solar InfraRed COronal Magnetograph (SIRCOM) Proposal for a space based coronagraph for vector magnetic field measurements Solar InfraRed COronal Magnetograph (SIRCOM) A joint proposal by PRL & ISAC for
More informationChapter 8 The Sun Our Star
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 8 The Sun
More informationSolar photosphere. Michal Sobotka Astronomical Institute AS CR, Ondřejov, CZ. ISWI Summer School, August 2011, Tatranská Lomnica
Solar photosphere Michal Sobotka Astronomical Institute AS CR, Ondřejov, CZ ISWI Summer School, August 2011, Tatranská Lomnica Contents General characteristics Structure Small-scale magnetic fields Sunspots
More informationMeasuring magnetic free energy in the solar atmosphere
Measuring magnetic free energy in the solar atmosphere Philip G Judge, High Altitude Observatory, National Center for Atmospheric Research. judge@ucar.edu Abstract: The purpose of this white paper is to
More information1 Structure of the coronal magnetic field
Magnetic Properties of the Solar Atmosphere (SolmeX Cosmic Vision Mission) 2010 NRC Decadal Survey White Paper Submitted by J.D. Moses for the SolmeX Consortium The structure and dynamics of the solar
More informationInstrumental Polarization of Telescopes on Alt-Azimuth and Equatorial Mounts
Project Documentation Report #0009 Revision #A Instrumental Polarization of Telescopes on Alt-Azimuth and Equatorial Mounts Christoph U. Keller 4 December 2002 Advanced Technology Solar Telescope 950 N.
More information9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is
1 9-1 The Sun s energy is generated by thermonuclear reactions in its core The Sun s luminosity is the amount of energy emitted each second and is produced by the proton-proton chain in which four hydrogen
More information1.3j describe how astronomers observe the Sun at different wavelengths
1.3j describe how astronomers observe the Sun at different wavelengths 1.3k demonstrate an understanding of the appearance of the Sun at different wavelengths of the electromagnetic spectrum, including
More informationThe importance of ground-based observations of the solar corona
The importance of ground-based observations of the solar corona J. Burkepile 1, S. Tomczyk 1, P. Nelson 1, A.G. dewijn 1, S. Sewell 1, D. Elmore 2, L. Sutherland 1, R. Summers 1, D. Kolinski 1, L. Sitongia
More informationThe Sun. Basic Properties. Radius: Mass: Luminosity: Effective Temperature:
The Sun Basic Properties Radius: Mass: 5 R Sun = 6.96 km 9 R M Sun 5 30 = 1.99 kg 3.33 M ρ Sun = 1.41g cm 3 Luminosity: L Sun = 3.86 26 W Effective Temperature: L Sun 2 4 = 4πRSunσTe Te 5770 K The Sun
More informationScience Objectives and Instrument Designs of the SOLAR-C Mission
Science Objectives and Instrument Designs of the SOLAR-C Mission Y. Suematsu (NAOJ); SOLAR-C Working Group Synergies between ground and space based solar research 1 st SOLARNET 3 rd EAST/ATST meeting Oslo,
More informationToward Interplanetary Space Weather: Strategies for Manned Missions to Mars
centre for fusion, space and astrophysics Toward Interplanetary Space Weather: Strategies for Manned Missions to Mars Presented by: On behalf of: Jennifer Harris Claire Foullon, E. Verwichte, V. Nakariakov
More informationSolar Observation using ALMA
Solar Observation using ALMA Sujin Kim ALMA EA Korean Node, KASI Content Science Target Cycle4 selection statistics: Sun Capability for Cycle5 Science Verification(SV) data - Single-dish observation -
More informationUsing This Flip Chart
Using This Flip Chart Sunspots are the first indicators that a storm from the Sun is a possibility. However, not all sunspots cause problems for Earth. By following the steps in this flip chart you will
More informationTurbulent Origins of the Sun s Hot Corona and the Solar Wind
Turbulent Origins of the Sun s Hot Corona and the Solar Wind Steven R. Cranmer Harvard-Smithsonian Center for Astrophysics Turbulent Origins of the Sun s Hot Corona and the Solar Wind Outline: 1. Solar
More informationMagnetic flux emergence on the Sun and Sun-like stars
Magnetic flux emergence on the Sun and Sun-like stars Matthias Rempel 1, Yuhong Fan 1, Aaron Birch 2, and Douglas Braun 2 February 13, 2009 Abstract For our understanding of stellar magnetic activity across
More informationMeasurements of Solar Magnetic Field in Huairou Solar Observing Station (HSOS)
Measurements of Solar Magnetic Field in Huairou Solar Observing Station (HSOS) DENG Yuanyong Key Laboratory of Solar Activity, National Astronomical Observatories, Chinese Academy of Sciences Solar Observations
More informationarxiv: v1 [astro-ph.sr] 25 May 2015
Does the variation of solar inter-network horizontal field follow sunspot cycle? arxiv:1505.06519v1 [astro-ph.sr] 25 May 2015 C. L. Jin & J. X. Wang Key Laboratory of Solar Activity, National Astronomical
More informationActive Regions in. Spectroscopy. (or: Time Variations on the Solar Surface observed by 2D Spectro-Polarimetrie
Active Regions in Spectroscopy (or: Time Variations on the Solar Surface observed by 2D Spectro-Polarimetrie Motivation Wavelets Observations A few software details Obstacles and Errors Outline Results
More informationSoftware for Interactively Visualizing Solar Vector Magnetograms of Udaipur Solar Observatory
J. Astrophys. Astr. (2008) 29, 107 111 Software for Interactively Visualizing Solar Vector Magnetograms of Udaipur Solar Observatory Sanjay Gosain, Sanjiv Tiwari, Jayant Joshi & P. Venkatakrishnan Udaipur
More informationMagnetohydrodynamic Simulations at IRSOL
1st Swiss SCOSTEP workshop, Oct. 4 5, 2016 Oeschger Centre, Bern Magnetohydrodynamic Simulations at IRSOL Oskar Steiner Istituto Ricerche Solari Locarno (IRSOL), Locarno-Monti, Switzerland Kiepenheuer-Institut
More informationD. McKenzie (NASA) 3. Questions and discussions 2018/5/24 1
Session 8. Next Generation Solar Physics Mission special session (17:35-18:40) Purpose: Share the latest status among the community 1. The NGSPM-SOT report and Japanese contributions to the NGSPM T. Shimizu
More informationSolar eruptive phenomena
Solar eruptive phenomena Andrei Zhukov Solar-Terrestrial Centre of Excellence SIDC, Royal Observatory of Belgium 26/01/2018 1 Eruptive solar activity Solar activity exerts continous influence on the solar
More informationarxiv: v1 [astro-ph.im] 28 Jan 2017
Polarization Modeling and Predictions for DKIST Part 1: Telescope and example instrument configurations. David M. Harrington a and Stacey R. Sueoka b a National Solar Observatory, 8 Kiopa a Street, Ste
More informationPTYS/ASTR 206. The Sun 3/1/07
The Announcements Reading Assignment Review and finish reading Chapter 18 Optional reading March 2006 Scientific American: article by Gene Parker titled Shielding Space Travelers http://en.wikipedia.org/wiki/solar_variability
More informationarxiv:astro-ph/ v1 26 Sep 2003
DRAFT VERSION FEBRUARY 17, 2011 Preprint typeset using L A TEX style emulateapj v. 11/12/01 arxiv:astro-ph/0309727v1 26 Sep 2003 SIMULTANEOUS VISIBLE AND INFRARED SPECTRO-POLARIMETRY OF A SOLAR INTERNETWORK
More informationEvolution of Twisted Magnetic Flux Ropes Emerging into the Corona
Evolution of Twisted Magnetic Flux Ropes Emerging into the Corona Yuhong Fan High Altitude Observatory, National Center for Atmospheric Research Collaborators: Sarah Gibson (HAO/NCAR) Ward Manchester (Univ.
More informationThe Solar Probe Plus Ground Based Network
The Solar Probe Plus Ground Based Network V4.0 November 8, 2015 White Paper Authors: N. A. Schwadron, T. Bastian, J. Leibacher, D. Gary, A. Pevtsov, M. Velli, J. Burkpile, N. Raouafi, C. Deforest SPP GBN
More informationarxiv: v1 [astro-ph.sr] 13 Jan 2010
Mem. S.A.It. Vol. 75, 282 c SAIt 2008 Memorie della Onthe3DStructureoftheMagneticFieldin Regions of Emerging Flux arxiv:1001.2108v1 [astro-ph.sr] 13 Jan 2010 A. Asensio Ramos 1,2 and J. Trujillo Bueno
More informationSPITZER SPACE TELESCOPE
SPITZER SPACE TELESCOPE The Rationale for Infrared Astronomy reveal cool states of matter explore the hidden Universe provide access to many spectral features probe the early life of the cosmos WANT TO
More informationGuidepost. Chapter 08 The Sun 10/12/2015. General Properties. The Photosphere. Granulation. Energy Transport in the Photosphere.
Guidepost The Sun is the source of light an warmth in our solar system, so it is a natural object to human curiosity. It is also the star most easily visible from Earth, and therefore the most studied.
More informationThe Sun Our Extraordinary Ordinary Star
The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the
More informationAn Overview of the Details
The Sun Our Extraordinary Ordinary Star 1 Guiding Questions 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the
More informationChapter 1. Introduction. 1.1 Why study the sun?
Chapter 1 Introduction 1.1 Why study the sun? The sun is an ordinary main-sequence star of spectral type G2V. From the human perspective it is the most important star in the universe. It provides the earth
More informationOn the 3D structure of the magnetic eld in regions of emerging ux
Mem. S.A.It. Vol. 81, 625 c SAIt 2010 Memorie della On the 3D structure of the magnetic eld in regions of emerging ux A. Asensio Ramos 1,2 and J. Trujillo Bueno 1,2,3 1 Instituto de Astrofísica de Canarias,
More informationInvestigating Molecular Hydrogen in Active Regions with IRIS
Investigating Molecular Hydrogen in Active Regions with IRIS Sarah A. Jaeggli1, Philip G. Judge2, Steven H. Saar3, Adrian N. Daw4, & The IRIS Team 1 Montana State University Altitude Observatory 3 Harvard-Smithsonian
More informationAIA DATA ANALYSIS OVERVIEW OF THE AIA INSTRUMENT
AIA DATA ANALYSIS OVERVIEW OF THE AIA INSTRUMENT SDO SUMMER SCHOOL ~ August 2010 ~ Yunnan, China Marc DeRosa (LMSAL) ~ derosa@lmsal.com WHAT IS SDO? The goal of Solar Dynamics Observatory (SDO) is to understand:
More informationSpectropolarimetry of a decaying sunspot penumbra
Spectropolarimetry of a decaying sunspot penumbra L.R. Bellot Rubio Instituto de Astrofísica de Andalucía (CSIC), Apartado 04, 18080 Granada, Spain; lbellot@iaa.es and A. Tritschler National Solar Observatory/Sacramento
More informationThe European Solar Telescope: project status
Mem. S.A.It. Suppl. Vol. 19, 67 c SAIt 2012 Memorie della Supplementi The European Solar Telescope: project status F. Zuccarello 1,2 and the EST team 1 Dipartimento di Fisica e Astronomia Universitá di
More informationAn Overview of the Details
Guiding Questions The Sun Our Extraordinary Ordinary Star 1. What is the source of the Sun s energy? 2. What is the internal structure of the Sun? 3. How can astronomers measure the properties of the Sun
More informationIRIS observation of penumbral microjets in the chromosphere and their transition region counterpart
IRIS observation of penumbral microjets in the chromosphere and their transition region counterpart Y. Katsukawa (NAOJ), Y. Kimura (Univ. of Tokyo) T. J. Okamoto (Nagoya Univ.), T. Tarbell (LMSAL) IRIS-4
More informationSolar-terrestrial relation and space weather. Mateja Dumbović Hvar Observatory, University of Zagreb Croatia
Solar-terrestrial relation and space weather Mateja Dumbović Hvar Observatory, University of Zagreb Croatia Planets Comets Solar wind Interplanetary magnetic field Cosmic rays Satellites Astronauts HELIOSPHERE
More informationThe Sun. The Sun Is Just a Normal Star 11/5/2018. Phys1411 Introductory Astronomy. Topics. Star Party
Foundations of Astronomy 13e Seeds Phys1411 Introductory Astronomy Instructor: Dr. Goderya Chapter 8 The Sun Star Party This Friday November 9 weather permitting. See the flyer for updates in case of cancellations
More informationThe Solar Chromosphere
1 / 29 The Solar Chromosphere Recent Advances in Determining the Magnetic Fine Structure Andreas Lagg Max-Planck-Institut für Sonnensystemforschung Katlenburg-Lindau, Germany Rocks n Stars 2012 2 / 29
More informationNext%Genera*on%Solar% Physics%Mission%% %
Next%Genera*on%Solar% Physics%Mission%% % Science%Objec*ves%Team Overview/Progress, Lyndsay,Fletcher Charter JAXA/ESA/NASA%are%looking%at%a%possible%mul*Flateral% mission Primary%role%of%SOT%is%to%develop%and%document%
More informationThe Magnetic Free Energy in Active Regions. Energetic Events on the Sun are Common - I
The Magnetic Free Energy in Active Regions T. Metcalf, K. D. Leka, D. Mickey, B. LaBonte, and L. Ryder Energetic Events on the Sun are Common - I A Coronal Mass Ejection (CME) Observed with SOHO/LASCO
More information9/13/18. ASTR 1040: Stars & Galaxies. Topics for Today and Tues. Nonvisible Light X-ray, UV, IR, Radio. SPITZER Infrared Telescope
ASTR 1040: Stars & Galaxies Solar Prominence from SOHO EIT Prof. Juri Toomre TAs: Ryan Horton, Loren Matilsky Lecture 6 Thur 13 Sept 2018 zeus.colorado.edu/astr1040-toomre Topics for Today and Tues Next
More informationThe General Properties of the Sun
Notes: The General Properties of the Sun The sun is an average star with average brightness. It only looks bright because it s so close. It contains 99% of the mass of the solar system. It is made of entirely
More informationThe Sun. The Sun. Bhishek Manek UM-DAE Centre for Excellence in Basic Sciences. May 7, 2016
The Sun Bhishek Manek UM-DAE Centre for Excellence in Basic Sciences May 7, 2016 Outline 1 Motivation 2 Resume of the Sun 3 Structure of the Sun - Solar Interior and Atmosphere 4 Standard Solar Model -
More informationObservations of Umbral Flashes
Proceedings of 12th Cambridge Workshop on Cool Stars, Stellar Systems, & The Sun, 2003 University of Colorado. Observations of Umbral Flashes L.H.M. Rouppe van der Voort 1, J.M. Krijger 2 Abstract. We
More informationKinematics and magnetic properties of a light bridge in a decaying sunspot
Kinematics and magnetic properties of a light bridge in a decaying sunspot M. Falco 1, J. M. Borrero 2, S.L. Guglielmino 1, P. Romano 3, R. Schlichenmaier 2, F. Zuccarello 1, S. Criscuoli 4, A. Cristaldi
More informationStudy of a Large Helical Eruptive Prominence Associated with Double CME on 21 April 2001
J. Astrophys. Astr. (2006) 27, 347 352 Study of a Large Helical Eruptive Prominence Associated with Double CME on 21 April 2001 Syed Salman Ali, Wahab Uddin & Ramesh Chandra Aryabhatta Research Institute
More informationNext Generation UV Coronagraph Instrumentation for Solar Cycle-24
J. Astrophys. Astr. (2008) 29, 321 327 Next Generation UV Coronagraph Instrumentation for Solar Cycle-24 John L. Kohl 1,, Rajmal Jain 2, Steven R. Cranmer 1, Larry D. Gardner 1, Anil K. Pradhan 3, John
More informationThe Large UV Optical IR survey telescope. Debra Fischer
The Large UV Optical IR survey telescope Debra Fischer Yale University How do we identify worlds that are most promising for life? Host star insolation determines the probability of retaining water. Habitable
More informationSolar EUV Spectral Irradiance: Measurements. Frank Eparvier
Solar EUV Spectral Irradiance: Measurements Frank Eparvier eparvier@colorado.edu Outline Introduction to Solar EUV Irradiance TIMED-SEE and SDO-EVE New Insights into EUV Sun from EVE The Future of EUV
More informationThe Evershed flow and the brightness of the penumbra. Luis R. Bellot Rubio Instituto de Astrofísica de Andalucía (CSIC) Granada, Spain
The Evershed flow and the brightness of the penumbra Instituto de Astrofísica de Andalucía (CSIC) Granada, Spain Sunspots: general appearance AR 8704, DOT (La Palma), G-band @ 0.2" Sunspot brightness:
More information