Overview of observational methods and instruments: spectrographs. Sergei Shestov
|
|
|
- Erik Horatio Carpenter
- 5 years ago
- Views:
Transcription
1 Overview of observational methods and instruments: spectrographs Sergei Shestov
2 7 Feb 2018 SIDC seminar: spectrographs 2
3 Outline Scientific importance of spectroscopic observations Solar spectra Methods & assumptions of spectroscopic analysis Layout of a generic spectrograph Types of spectrographs: Slit spectrograph Slitless spectrographs Crystal spectrographs Photometers Solid state spectrographs Literature 7 Feb 2018 SIDC seminar: spectrographs 3
4 7 Feb 2018 SIDC seminar: spectrographs 4
5 Some facts about spectroscopic observations Bohr s model of the Hydrogen atom (1913); Hubble s law (1927, based on V. Splipher redshifts); Solar corona: determination of temperature (Edlen, 1942), chemical composition; Atomic physics: atomic structure (diel. satellites), precise energy levels (the IRON project) 7 Feb 2018 SIDC seminar: spectrographs 5
6 Solar corona spectrum Blackbody T=5762 K in whitelight (thermodynamic eq.); Charged ions emit spectral lines and continuum as a result of excitation; Bremsstrahlung emission of electrons; 7 Feb 2018 SIDC seminar: spectrographs 6
7 Bohr atom model, Hlike atoms H Z=1 ~ 1215 Å He II Z=2 ~ 304 Å Mg XII Z=12 ~ 8.42 Å Fe XXVI Z=26 ~ 1.80 Å Fe IX Å: 3p 6 1 S 0 < 3p 5 3d 1 P 1 ; Fe XII Å: 3s 2 3p 3 4 S 3/2 < 3s 2 3p 2 (3p) 3d 4 P 5/2 7 Feb 2018 SIDC seminar: spectrographs 7
8 Methods of spectroscopic analysis j I hν ~ N X,m j N X,m A ji g ~ N X,m N e ~ Ab X f(t, n e ) N H N e T, n e hν I hν ~Ab X f T, n e A ji N H N e Intensities of individual lines distribution of T, n e ; Spectral line shape T, presence of flows; 7 Feb 2018 SIDC seminar: spectrographs 8
9 Necessary simplifications I hν ~ Ab X f T, n e A ji N H N e Optically thin Ionization equilibria Electron excitation are more frequent T, n e hν 7 Feb 2018 SIDC seminar: spectrographs 9
10 Necessary simplifications H α spectral line I hν ~ Ab X f T, n e A ji N H N e Optically thin Ionization equilibria Electron excitation are more frequent T, n e hν 7 Feb 2018 SIDC seminar: spectrographs 10
11 Generic layout of a spectrograph Entrance slit Collimator Dispersive element (prism) Objective Detector 7 Feb 2018 SIDC seminar: spectrographs 11
12 Types of spectrograph Diffraction grating based Slit Slitless Photometers Crystal based Solid state based down to 30 Å; Å; Å; Si kev (0.830 Å); Ge 4 kev17 MeV; EIS/Hinode; CDS, SUMER (SOHO); SERTS; VAULT; IRIS Skylab S082A; SPIRIT/CORONASF; EVE/SDO; Lyra/PROBA2; GOES SXR; RESIK, DIOGENESS, Mg XII (CORONASF); BCS, FCS (SMM); BCS/Yohkoh; SphinX/CORONASPHOTON; RHESSI; SOXT; 7 Feb 2018 SIDC seminar: spectrographs 12
13 Slit spectrograph EUV & UV spectral range 7 Feb 2018 SIDC seminar: spectrographs 13
14 IRIS UV spectrograph 7 Feb 2018 SIDC seminar: spectrographs 14
15 SUMER/SOHO CDS/SOHO EIS/Hinode IRIS SERTS SPICE/Sol.Orb Å Å , Å , , Å , Å , Å FUV spectra from IRIS (Tian et al. 2015) Monochromatic image Fe XII Å from EIS/Hinode Doppler shift map 7 Feb 2018 SIDC seminar: spectrographs 15
16 Pros & Cons slit spectrographs High spectral resolution & spatial resolution in direction; Spectra of small regions covered by the slit or slot; Impossible to get simultaneous spectra of the whole Sun scanning; Large amount of optics small sensitivity; Save the whales photons! 7 Feb 2018 SIDC seminar: spectrographs 16
17 Spectroheliograph EUV & UV spectral range 7 Feb 2018 SIDC seminar: spectrographs 17
18 Spectroheliograph EUV & UV spectral range 7 Feb 2018 SIDC seminar: spectrographs 18
19 Spectroheliograph EUV & UV spectral range 7 Feb 2018 SIDC seminar: spectrographs 19
20 S082A spectroheliograph on Skylab A; Concave grating; Photographic film; 7 Feb 2018 SIDC seminar: spectrographs 20
21 SPIRIT EUV spectoheliograph on CORONASF , A; Plane grating, grazing incidence; Multilayer mirror & CCDbased detector 7 Feb 2018 SIDC seminar: spectrographs 21
22 Pros & Cons spectroheliographs FullSun spectral images; Higher sensitivity? Possibility for high corona observations; Lower spatial resolution WRT slit spectrographs; Monochromatic images are overlapping overlapograms; Difficult to analyze data; Future: COSIE for the ISS CfA, for the high corona observations KORTES for the ISS LPI, studying of flaring plasma 7 Feb 2018 SIDC seminar: spectrographs 22
23 EUV slit spectrograph with no imaging EVE/SDO 7 Feb 2018 SIDC seminar: spectrographs 23
24 EUV slit spectrograph with no imaging EVE/SDO 7 Feb 2018 SIDC seminar: spectrographs 24
25 Pros & Cons No spatial resolution average spectrum of the Sun; Very wide spectral bandwidth; High temporal resolution; High sensitivity; 7 Feb 2018 SIDC seminar: spectrographs 25
26 Crystal spectrograph Low λ impossible (almost) to use diffraction gratings; Crystals BraggWulf law: nλ = 2d sin λ 7 Feb 2018 SIDC seminar: spectrographs 26
27 Crystal spectrograph Low λ Bent crystal impossible (almost) to use diffraction gratings; Crystals BraggWulf law: nλ = 2d sin λ Mission Instrument Spectral range, A Crystal Solar Maximum Mission BCS Ge 422 spectrometer FCS Ge 220 CORONASF DIOGENESS Quartz ADP Beryl Quartz 1010 RESIK Si Quartz 1010 Yohkoh BCS Ge 222 Hinotori Intercosmos Bragg crustal spectrometer Ge Ge 111 P78 7 Feb 2018 SIDC seminar: spectrographs 27
28 Flat and Bentcrystal spectrographs BCS/Yohkoh ( ) Å 7 Feb 2018 SIDC seminar: spectrographs 28
29 RESIK flare spectra RESIK/CORONASF ( ) Å 7 Feb 2018 SIDC seminar: spectrographs 29
30 RESIK flare spectra RESIK/CORONASF ( ) Å Chifor et al. 2007; C5.8 flare 22 Feb Feb 2018 SIDC seminar: spectrographs 30
31 Mg XII spectroheliograph 8.42 Å Crystal quartz mirror [10 1 0] Detector CCD 2d=8.501 > BraggWulf > λ=8.42 Å 7 Feb 2018 SIDC seminar: spectrographs 31
32 Emissivity Mg XII 8.42 Å Mg XII spectroheliograph 8.42 Å 7 Feb 2018 SIDC seminar: spectrographs 32
33 Pros & Cons crystal spectrographs Soft Xray wavelength; Limited set of crystals available; Imaging capabilities are limited; Really see hot plasma; Future: ChemiX for the InterhelioProbe SRC, Wroclaw SolPex for the ISS SRC&LPI MaGIXS from MSFC 7 Feb 2018 SIDC seminar: spectrographs 33
34 MaGIXS spectrograph for Soft Xray Telescope Slit Collimator Diffraction grating CCD detector Slit soft Xray spectrograph; Å spectral range ( kev); Grazing incidence diffraction grating; Wolter type I telescope; Grazing incidence collimator; CCD detector; MaGIXS Marshall Grazing Incidence Xray Spectrometer 7 Feb 2018 SIDC seminar: spectrographs 34
35 Photometers Lyra/PROBA2 GOES SXR detectors Å Å 1800 Å 1200 Å; 0.54 Å 18 Å; Detector Filters Solar flux 7 Feb 2018 SIDC seminar: spectrographs 35
36 GOES SXR detectors Series of satellites since 1974; Two ion chamber based SXR detectors; Different response of two detectors > Diagnostics of plasma T, EM (White et al. 2005) 7 Feb 2018 SIDC seminar: spectrographs 36
37 Pros & Cons photometers Relatively simple to build; Relatively difficult to interpret data, due to registering of average signal in some passband; 7 Feb 2018 SIDC seminar: spectrographs 37
38 Solid state spectrographs Due to absorption in semiconductor a photon creates charge in the valence zone; For Si 3.6 ev per eh pair, e.g Å = 1.47 kev > 410 e SphinX/CORONASPHOTON Si photodiodes, kev RHESSI Ge detectors, 4320 kev; SOXT 425 kev Si, 456 CdZnTe; STIX/Sol.Orb. CdTe detectors, 4150 kev 7 Feb 2018 SIDC seminar: spectrographs 38
39 SphinX soft Xray spectrometer SphinX/CORONASPHOTON XRT/Hinode TESIS/CORONASPHOTON 7 Feb 2018 SIDC seminar: spectrographs 39
40 RHESSI T~30 MK T~10 MK Bremsstrahlung from energetic electrons Decay of pions 7 Feb 2018 SIDC seminar: spectrographs 40
41 Pros & Cons solid state spectorgraphs Possibility to go to higher energies; High cadence; No spatial resolution? Low spectral resolution; 7 Feb 2018 SIDC seminar: spectrographs 41
42 Thank you! 7 Feb 2018 SIDC seminar: spectrographs 42
43 Literature K. Phillips, U. Feldman, E. Landi Ultraviolet and Xray Spectroscopy of the Solar Atmosphere Doschek, G. A., & Feldman, U. (2010). The solar UV xray spectrum from 1.5 to 2000 Å CHIANTI atomic database documentation M. J. Aschwanden, Physics of the Solar Corona. An Introduction Chapter 2 Mason, H. E., & Monsignori Fossi, B. C. (1994). Spectroscopic diagnostics in the VUV for solar and stellar plasmas 7 Feb 2018 SIDC seminar: spectrographs 43
44 7 Feb 2018 SIDC seminar: spectrographs 44
45 7 Feb 2018 SIDC seminar: spectrographs 45
46 7 Feb 2018 SIDC seminar: spectrographs 46
47 7 Feb 2018 SIDC seminar: spectrographs 47
48 AIA channels and composites; HMIB 7 Feb 2018 SIDC seminar: spectrographs 48
49 AIA thermal responses 7 Feb 2018 SIDC seminar: spectrographs 49
50 7 Feb 2018 SIDC seminar: spectrographs 50
51 7 Feb 2018 SIDC seminar: spectrographs 51
52 7 Feb 2018 SIDC seminar: spectrographs 52
Solar UV Spectroscopy and Coronagraphy
Solar UV Spectroscopy and Coronagraphy Werner Curdt Outline motivation the Sun s electromagnetic spectrum spectroscopic methods observational examples instrumental aspects optical design detectors others
Janusz Sylwester & Barbara Sylwester Space Research Centre Polish Academy of Sciences, Wrocław, Poland
Janusz Sylwester & Barbara Sylwester Space Research Centre Polish Academy of Sciences, Wrocław, Poland Ken Phillips Mullard Space Science Laboratory University College London and V.D. Kuznetsov Pushkov
Discovery of Emission Lines in the X-ray Spectrum of the Perseus Cluster
Discovery of Emission Lines in the X-ray Spectrum of the Perseus Cluster J. L. Culhane University College London Mullard Space Science Laboratory Summary Nature of the Solar Corona and properties of its
Solar X-rays from 0.3 A.U.: the CherniX Bragg Spectrometer on Interhelioprobe
Solar and Stellar Flares and their Effects on Planets Proceedings IAU Symposium No. 320, 2015 International Astronomical Union 2016 A.G. Kosovichev, S.L. Hawley & P. Heinzel, eds. doi:10.1017/s1743921316000338
SOLAR SOFT X- RAY EXPERIMENTS UNDER DEVELOPMENT AT THE SOLAR PHYSICS DIVISION OF SPACE RESEARCH CENTRE POLISH ACADEMY OF SCIENCES WROCLAW
SOLAR SOFT X- RAY EXPERIMENTS UNDER DEVELOPMENT AT THE SOLAR PHYSICS DIVISION OF SPACE RESEARCH CENTRE POLISH ACADEMY OF SCIENCES WROCLAW Our Team & heritage Funded instrument projects Instruments under
Date of delivery: 5 May 2016 Journal and vol/article ref: IAU Number of pages (not including this page): 3
Proof Delivery Form Proceedings of the International Astronomical Union Date of delivery: 5 May 2016 Journal and vol/article ref: IAU 1600031 Number of pages (not including this page): 3 This proof is
DETERMINATION OF HOT PLASMA CHARACTERISTICS FROM TRACE IMAGES. S. Gburek 1 and T. Mrozek 2
DETERMINATION OF HOT PLASMA CHARACTERISTICS FROM TRACE IMAGES. S. Gburek 1 and T. Mrozek 2 1 Space Research Centre, Polish Academy of Sciences, Solar Physics Division, 51-622 Wroclaw, ul. Kopernika 11,
High-temperature solar flare plasma behaviour from crystal spectrometer observations
Solar and Stellar Flares and their Effects on Planets Proceedings IAU Symposium No. 0, 05 International Astronomical Union 06 A.G. Kosovichev, S.L. Hawley & P. Hemzel, eds. doi:0.07/s7960000 High-temperature
OUTLINE: P. Kotrč (1), P. Heinzel (1) and O. Procházka (2)
On measurements of continuum flux in solar flares. Instrument and first results. P. Kotrč (1), P. Heinzel (1) and O. Procházka (2) (1) - Astronomical Institute, AS CR, v.v.i. Ondřejov, Czech Republic (2)
CHIANTI An atomic database for astrophysical plasmas
CHIANTI An atomic database for astrophysical plasmas Enrico Landi University of Michigan On behalf of the CHIANTI team: Enrico Landi Ken Dere Peter Young Giulio Del Zanna Helen Mason University of Michigan,
2 The solar atmosphere
1 The solar atmosphere 1.1 Introduction The solar atmosphere may be broadly defined as that part of the Sun extending outwards from a level known as the photosphere where energy generated at the Sun s
Spectroscopic analysis of the solar flare event on 2002 August 3 with the use of RHESSI and RESIK data
Available online at www.sciencedirect.com Advances in Space Research 42 (2008) 822 827 www.elsevier.com/locate/asr Spectroscopic analysis of the solar flare event on 2002 August 3 with the use of RHESSI
Solar radiation and plasma diagnostics. Nicolas Labrosse School of Physics and Astronomy, University of Glasgow
Solar radiation and plasma diagnostics Nicolas Labrosse School of Physics and Astronomy, University of Glasgow 0 Radiation basics Radiation field in the solar atmosphere Amount of radiant energy flowing
Chapter 4. Spectroscopy. Dr. Tariq Al-Abdullah
Chapter 4 Spectroscopy Dr. Tariq Al-Abdullah Learning Goals: 4.1 Spectral Lines 4.2 Atoms and Radiation 4.3 Formation of the Spectral Lines 4.4 Molecules 4.5 Spectral Line Analysis 2 DR. T. AL-ABDULLAH
LINE INTENSITY RATIOS IN THE EIS RANGE SENSITIVE TO ELECTRON DENSITIES IN 10 7 K PLASMAS
The Astrophysical Journal, 679:843Y847, 2008 May 20 # 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A. LINE INTENSITY RATIOS IN THE EIS RANGE SENSITIVE TO ELECTRON DENSITIES
Spectroscopy in Astronomy
Spectroscopy in Astronomy History 1814 German optician Joseph von Fraunhofer sun with 600+ spectral lines; now we know more than 3000 lines 1860 German chemists Gustav Kirchhoff and Robert W. Bunsen Chemical
X-Ray Photoelectron Spectroscopy (XPS)
X-Ray Photoelectron Spectroscopy (XPS) Louis Scudiero http://www.wsu.edu/~scudiero; 5-2669 Electron Spectroscopy for Chemical Analysis (ESCA) The basic principle of the photoelectric effect was enunciated
DETERMINATION OF THE FORMATION TEMPERATURE OF Si IV IN THE SOLAR TRANSITION REGION
THE ASTROPHYSICAL JOURNAL, 477 : L119 L122, 1997 March 10 1997. The American Astronomical Society. All rights reserved. Printed in U.S.A. DETERMINATION OF THE FORMATION TEMPERATURE OF Si IV IN THE SOLAR
pre 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
Soft X-ray polarimeter-spectrometer SOLPEX
Solar and Stellar Flares and their Effects on Planets Proceedings IAU Symposium No. 320, 2015 International Astronomical Union 2016 A.G. Kosovichev, S.L. Hawley & P. Heinzel, eds. doi:10.1017/s1743921316002106
Dynamic 10 MK plasma structures observed in monochromatic full-sun images by the SPIRIT spectroheliograph on the CORONAS-F mission
Mon. Not. R. Astron. Soc. 338, 67 71 (2003) Dynamic 10 MK plasma structures observed in monochromatic full-sun images by the SPIRIT spectroheliograph on the CORONAS-F mission I. A. Zhitnik, 1 O. I. Bugaenko,
Your article is published under the Creative Commons Attribution license which allows users to read, copy, distribute and make derivative works, as
1 23 Your article is published under the Creative Commons Attribution license which allows users to read, copy, distribute and make derivative works, as long as the author of the original work is cited.
X-Ray Photoelectron Spectroscopy (XPS)
X-Ray Photoelectron Spectroscopy (XPS) Louis Scudiero http://www.wsu.edu/~scudiero; 5-2669 Fulmer 261A Electron Spectroscopy for Chemical Analysis (ESCA) The basic principle of the photoelectric effect
X-Rays From Laser Plasmas
X-Rays From Laser Plasmas Generation and Applications I. C. E. TURCU CLRC Rutherford Appleton Laboratory, UK and J. B. DANCE JOHN WILEY & SONS Chichester New York Weinheim Brisbane Singapore Toronto Contents
Possible stereoscopic Hard X-ray observations with STIX and SORENTO instruments
Possible stereoscopic Hard X-ray observations with STIX and SORENTO instruments Tomasz Mrozek 1,2 1 Space Research Centre, Polish Academy of Sciences, Solar Physics Division 2 Astronomical Institute, University
Date of delivery: 5 May 2016 Journal and vol/article ref: IAU Number of pages (not including this page): 4
Proof Delivery Form Proceedings of the International Astronomical Union Date of delivery: 5 May 2016 Journal and vol/article ref: IAU 1600050 Number of pages (not including this page): 4 This proof is
A new concept of Balmer continuum flux measurement in solar flares
A new concept of Balmer continuum flux measurement in solar flares P. Kotrč, P. Heinzel and M. Zapior Astronomical Institute, AS CR, v.v.i. Ondřejov, Czech Republic Introduction White light flares, Balmer/blue
X-ray observations of Solar Flares. Marina Battaglia Fachhochschule Nordwestschweiz (FHNW)
X-ray observations of Solar Flares Marina Battaglia Fachhochschule Nordwestschweiz (FHNW) marina.battaglia@fhnw.ch 2 3 The solar corona Close by astrophysical laboratory allows us to study: Release of
arxiv: v1 [astro-ph] 28 Oct 2008
![arxiv: v1 [astro-ph] 28 Oct 2008](/thumbs/92/108661452.jpg "arxiv: v1 [astro-ph] 28 Oct 2008")
New EUV Fe IX emission line identifications from Hinode/EIS P. R. Young Space Science Division, Naval Research Laboratory, Washington, DC 20375 arxiv:0810.5028v1 [astro-ph] 28 Oct 2008 George Mason University,
A benchmark study for CHIANTI based on RESIK solar flare spectra ABSTRACT
A&A 462, 323 330 (2007) DOI: 10.1051/0004-6361:20066261 c ESO 2007 Astronomy & Astrophysics A benchmark study for CHIANTI based on RESIK solar flare spectra C. Chifor 1,G.DelZanna 2,H.E.Mason 1, J. Sylwester
Overview: Astronomical Spectroscopy
Overview: Astronomical Spectroscopy or How to Start Thinking Creatively about Measuring the Universe Basic Spectrograph Optics Objective Prism Spectrometers - AESoP Slit Spectrometers Spectrometers for
Spectral signatures of the impulsive energy release in SMM BCS spectra
Spectral signatures of the impulsive energy release in SMM BCS spectra B. Sylwester, J. Sylwester, K.J.H. Phillips, A. Kępa, Ż. Szaforz Space Research Center of PAS, Wrocław Earth Sciences Department,
Temperature Reconstruction from SDO:AIA Filter Images
Temperature Reconstruction from SDO:AIA Filter Images A report by Chris Gilbert Astrophysical and Planetary Sciences, University of Colorado Boulder ASTR 5700; Stellar Astrophysics, Spring 2016 Abstract
Solar Flare Variations
Solar Flare Variations Advisors: Phillip Chamberlin, Rachel Hock and Tom Woods NSF By Chris Moore Outline Overview of solar activity Relevance Proxies Halloween flares Procedures Analysis Conclusion Goals
Astr 2310 Thurs. March 3, 2016 Today s Topics
Astr 2310 Thurs. March 3, 2016 Today s Topics Chapter 6: Telescopes and Detectors Optical Telescopes Simple Optics and Image Formation Resolution and Magnification Invisible Astronomy Ground-based Radio
Problem Solving. radians. 180 radians Stars & Elementary Astrophysics: Introduction Press F1 for Help 41. f s. picture. equation.
Problem Solving picture θ f = 10 m s =1 cm equation rearrange numbers with units θ factors to change units s θ = = f sinθ fθ = s / cm 10 m f 1 m 100 cm check dimensions 1 3 π 180 radians = 10 60 arcmin
AIA 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:
Flare Irradiance Spectral Model (FISM) use for space weather applications
Flare Irradiance Spectral Model (FISM) use for space weather applications P. C. Chamberlin, T. N. Woods and F. G. Eparvier Laboratory for Atmospheric and Space Physics, University of Colorado, 1234 Innovation
X-ray Imaging & Spectral Statistics of Small Solar Flares Observed with RHESSI
X-ray Imaging & Spectral Statistics of Small Solar Flares Observed with RHESSI Iain G. Hannah Steven Christe, Säm Krucker, Gordon Hurford, Hugh Hudson & Robert P. Lin Space Sciences Laboratory, University
J. Sylwester, B. Sylwester, Ken Phillips b, A. Kępa
J. Sylwester, B. Sylwester, Ken Phillips b, A. Kępa Space Research Centre Polish Academy of Sciences, Wrocław, Poland and b Natural History Museum, London eheroes annual meeting, Leuven: 7-9 January 2015
Date of delivery: 5 May 2016 Journal and vol/article ref: IAU Number of pages (not including this page): 3
Proof Delivery Form Proceedings of the International Astronomical Union Date of delivery: 5 May 2016 Journal and vol/article ref: IAU 1600209 Number of pages (not including this page): 3 This proof is
25 Instruments for Optical Spectrometry
25 Instruments for Optical Spectrometry 25A INSTRUMENT COMPONENTS (1) source of radiant energy (2) wavelength selector (3) sample container (4) detector (5) signal processor and readout (a) (b) (c) Fig.
Optical/IR Observational Astronomy Spectroscopy. David Buckley, SALT
David Buckley, SALT 1 Background is really just monochromatic photometry History 1637 Descartes explained the origin of the rainbow. 1666 Newton s classic experiments on the nature of colour. 1752 Melvil
arxiv: v1 [astro-ph.sr] 14 Jan 2010
![arxiv: v1 [astro-ph.sr] 14 Jan 2010](/thumbs/71/65954534.jpg "arxiv: v1 [astro-ph.sr] 14 Jan 2010")
THE SOLAR X-RAY CONTINUUM MEASURED BY RESIK K. J. H. Phillips 1 arxiv:1001.2412v1 [astro-ph.sr] 14 Jan 2010 Mullard Space Science Laboratory, University College London, Holmbury St Mary, Dorking, Surrey
EUV-XUV Spectroscopic Technology and Instrumentation
EUV-XUV Spectroscopic Technology and Instrumentation Environmental physical conditions (plasma parameters, fields, particles.) affect atomic and ion inner fields (i.e. energy levels: broadening, shifting,
Why Go To Space? Leon Golub, SAO BACC, 27 March 2006
Why Go To Space? Leon Golub, SAO BACC, 27 March 2006 Solar Observation Observation of the Sun has a long and distinguished history Especially important as calendar where e.g. seasonal monsoons produced
Temporal evolution of differential emission measure and electron distribution function in solar flares based on joint RHESSI and SDO observations
Temporal evolution of differential emission measure and electron distribution function in solar flares based on joint RHESSI and SDO observations Galina G. Motorina 1 and Eduard P. Kontar 2 1 Pulkovo Observatory,
Solar Orbiter/SPICE: composition studies
Solar Orbiter/SPICE: composition studies Alessandra Giunta 1-2/10/2015 - ADAS workshop 1 Solar Orbiter/SPICE Door Mechanism Grating Assembly Particle Deflector SPICE Slit Change Mechanism Mirror & Scan
Downflow as a Reconnection Outflow
The Solar-B Mission and the Forefront of Solar Physics ASP Conference Series, Vol. 325, 2004 T. Sakurai and T. Sekii, eds. Downflow as a Reconnection Outflow Ayumi Asai and Kazunari Shibata Kwasan and
EMISSION SPECTROSCOPY
IFM The Department of Physics, Chemistry and Biology LAB 57 EMISSION SPECTROSCOPY NAME PERSONAL NUMBER DATE APPROVED I. OBJECTIVES - Understand the principle of atomic emission spectra. - Know how to acquire
9/13/18. 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
Phillip Chamberlin NASA Goddard Space Flight Center Solar Physics Laboratory Greenbelt, MD USA
Phillip Chamberlin NASA Goddard Space Flight Center Solar Physics Laboratory Greenbelt, MD USA Phillip.C.Chamberlin@NASA.gov With important contributions from Ryan Milligan (QUB), Daniel Ryan (ROB), Jan
Common SphinX & RHESSI observations of solar flares
Common SphinX & RHESSI observations of solar flares Mrozek, T. 1,2, Sylwester, J. 1, Siarkowski, M. 1, Sylwester, B. 1, Gburek, S. 1, Kępa,A. 1 1 Solar Physics Division, Space Research Centre, Polish Academy
AS 101: Day Lab #2 Summer Spectroscopy
Spectroscopy Goals To see light dispersed into its constituent colors To study how temperature, light intensity, and light color are related To see spectral lines from different elements in emission and
Solar-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
arxiv: v1 [astro-ph.sr] 3 Mar 2015
![arxiv: v1 [astro-ph.sr] 3 Mar 2015](/thumbs/73/68870949.jpg "arxiv: v1 [astro-ph.sr] 3 Mar 2015")
RESIK SOLAR X-RAY FLARE ELEMENT ABUNDANCES ON A NON-ISOTHERMAL ASSUMPTION arxiv:1503.00979v1 [astro-ph.sr] 3 Mar 2015 B. Sylwester 1, K. J. H. Phillips 2, J. Sylwester 1, and A. Kępa 1 1 Space Research
Study of Electron Energy and Angular Distributions and Calculations of X-ray, EUV Line Flux and Rise Times
J. Astrophys. Astr. (1987) 8, 263 270 Study of Electron Energy and Angular Distributions and Calculations of X-ray, EUV Line Flux and Rise Times Ranjna Bakaya, Sunil Peshin, R. R. Rausaria & P. N. Khosa
Chapter 8. Spectroscopy. 8.1 Purpose. 8.2 Introduction
Chapter 8 Spectroscopy 8.1 Purpose In the experiment atomic spectra will be investigated. The spectra of three know materials will be observed. The composition of an unknown material will be determined.
PRESENT STATUS OF RESEARCH AT THE WROCLAW SOLAR PHYSICS DIVISION OF SPACE RESEARCH CENTRE PAS. Janusz Sylwester
PRESENT STATUS OF RESEARCH AT THE WROCLAW SOLAR PHYSICS DIVISION OF SPACE RESEARCH CENTRE PAS Janusz Sylwester 15th UKRAINIAN CONFERENCE ON SPACE RESEARCH ODESA, UKRAINE: August 24 28, 2015 Outline History
Identifying Emission Lines in the Solar Extreme Ultraviolet (EUV) Irradiance Spectrum
Identifying Emission Lines in the Solar Extreme Ultraviolet (EUV) Irradiance Spectrum Rachael L. Tomasino Advisors: Dr. Frank Eparvier and Rachel Hock University of Colorado, Boulder Laboratory for Atmospheric
Spectroscopy. AST443, Lecture 14 Stanimir Metchev
Spectroscopy AST443, Lecture 14 Stanimir Metchev Administrative Homework 2: problem 5.4 extension: until Mon, Nov 2 Homework 3: problems 8.32, 8.41, 10.31, 11.32 of Bradt due in class Mon, Nov 9 Reading:
Nearly everything I need to know about. Observing the Sun. I learned from Halliday & Resnick. Charles Kankelborg Solar Physics REU Program
Nearly everything I need to know about Observing the Sun I learned from Halliday & Resnick Charles Kankelborg 2010 Solar Physics REU Program David Halliday David Halliday died April 2, 2010 in Maple Falls,
Astrophysics, Cambridge, MA, USA; 3 Southwest Research Institute, Boulder, CO, USA; 4 Catholic University, Washington, DC, USA
Solving the Coronal Heating Problem using X-ray Microcalorimeters S. Christe 1, S. Bandler 1, E. DeLuca 2, A. Caspi 3, L. Golub 2, R. Smith 2, J. Allred 1, J. W. Brosius 4, B. Dennis 1, J. Klimchuk 1 1
Extreme ultraviolet spectroscopy of highly charged argon ions at the Berlin EBIT
Extreme ultraviolet spectroscopy of highly charged argon ions at the Berlin EBIT C. Biedermann, R. Radtke, G. Fussmann, F.I. Allen Institut für Physik der Humboldt-Universität zu Berlin, Lehrstuhl Plasmaphysik,
Bragg spectroscopy from CORONAS-F
Multi-Wavelength Investigations of Solar Activity Proceedings IAU Symposium No. 223, 2004 c 2004 International Astronomical Union A.V. Stepanov, E.E. Benevolenskaya & A.G. Kosovichev, eds. DOI: 10.1017/S1743921304006337
Supporting Calculations for NASA s IRIS Mission. I. Overview
Supporting Calculations for NASA s IRIS Mission. I. Overview Eugene Avrett Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138 Understanding the solar chromosphere continues
ASTR-1010: Astronomy I Course Notes Section IV
ASTR-1010: Astronomy I Course Notes Section IV Dr. Donald G. Luttermoser Department of Physics and Astronomy East Tennessee State University Edition 2.0 Abstract These class notes are designed for use
Spectroscopy for planetary upper atmospheres きょくたん
Spectroscopy for planetary upper atmospheres きょくたん Spectrum of Venus atmosphere Spectrum of Jupiter and Io Figure 1. An EUV spectrum measured by Hisaki spacecraft. The spectrograph mixes spatial and spectral
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES
THE OBSERVATION AND ANALYSIS OF STELLAR PHOTOSPHERES DAVID F. GRAY University of Western Ontario, London, Ontario, Canada CAMBRIDGE UNIVERSITY PRESS Contents Preface to the first edition Preface to the
SPECTRAL ATLAS OF X-RAY LINES EMITTED DURING SOLAR FLARES BASED ON CHIANTI
The Astrophysical Journal Supplement Series, 160:286 311, 2005 September # 2005. The American Astronomical Society. All rights reserved. Printed in U.S.A. SPECTRAL ATLAS OF X-RAY LINES EMITTED DURING SOLAR
Spectroscopic studies of impurities in the LHD plasmas
Spectroscopic studies of impurities in the LHD plasmas Visitor: Zhenwei Wu (the institute of plasma physics, CAS -ASIPP) Host: Shigeru Morita (the national institute for fusion science -NIFS) Content 1.
Spectroscopic Diagnostics of the Solar Coronal Plasma
ISSN 1063-780X, Plasma Physics Reports, 2014, Vol. 40, No. 11, pp. 855 892. Pleiades Publishing, Ltd., 2014. Original Russian Text V.A. Slemzin, F.F. Goryaev, S.V. Kuzin, 2014, published in Fizika Plazmy,
AG Draconis. A high density plasma laboratory. Dr Peter Young Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B.
AG Draconis A high density plasma laboratory Collaborators A.K. Dupree S.J. Kenyon B. Espey T.B. Ake p.r.young@rl.ac.uk Overview CHIANTI database Symbiotic Stars AG Draconis FUSE FUSE observations of AG
Modern observational techniques for coronal studies
Modern observational techniques for coronal studies Hardi Peter Kiepenheuer-Institut für Sonnenphysik Freiburg solar eclipse, 11.8.1999, Wendy Carlos and John Kern The spectrum of the Sun RADIO observing
Physik und Anwendungen von weicher Röntgenstrahlung I (Physics and applications of soft X-rays I)
Physik und Anwendungen von weicher Röntgenstrahlung I (Physics and applications of soft X-rays I) Sommersemester 2015 Veranstalter : Prof. Dr. Ulf Kleineberg (ulf.kleineberg@physik.uni-muenchen.de) LMU,
Solar Spectroscopy. with Hinode/EIS and IRIS. Magnus Woods With thanks to David Long UCL-Mullard Space Science Laboratory
Solar Spectroscopy with Hinode/EIS and IRIS 4 th Solarnet Workshop, Mullard Space Science Laboratory Magnus Woods With thanks to David Long UCL-Mullard Space Science Laboratory magnus.woods.15@ucl.ac.uk
Course Details. Analytical Techniques Based on Optical Spectroscopy. Course Details. Textbook. SCCH 211: Analytical Chemistry I
SCCH 211: Analytical Chemistry I Analytical Techniques Based on Optical Spectroscopy Course Details September 22 October 10 September 22 November 7 November 17 December 1 Topic Period Introduction to Spectrometric
Plasma Radiation. Ø Free electrons Blackbody emission Bremsstrahlung
Plasma Radiation Ø Free electrons Blackbody emission Bremsstrahlung Ø Bound electrons (Z>2) Unresolved, multi-line emission Resolved line emission -- Single Z +n Objective Infer a thermodynamic quantity
SISD Training Lectures in Spectroscopy
SISD Training Lectures in Spectroscopy Anatomy of a Spectrum Visual Spectrum of the Sun Blue Spectrum of the Sun Morphological Features in Spectra λ 2 Line Flux = Fλ dλ λ1 (Units: erg s -1 cm -2 ) Continuum
TRACE DOWNFLOWS AND ENERGY RELEASE
TRACE DOWNFLOWS AND ENERGY RELEASE Ayumi Asai (1), T. Yokoyama (2), M. Shimojo (3), R. TanDokoro (4), M. Fujimoto (4), and K. Shibata (1) (1 ) Kwasan and Hida Observatories, Kyoto University, Kyoto, 607-8471
New Solar Irradiance Measurements from the Miniature X-Ray Solar Spectrometer CubeSat
New Solar Irradiance Measurements from the Miniature X-Ray Solar Spectrometer CubeSat Thomas N. Woods 1, Amir Caspi 2, Phillip C. Chamberlin 3, Andrew Jones 1, Richard Kohnert 1, James Paul Mason 1, Christopher
Matthew Lewis. Final Report
Final Report An investigation to determine how accurately the two broad band X-ray measurements from the NASA geostationary operational environmental satellite (GOES) can reproduce the full X-ray spectrum
TESIS experiment on EUV imaging spectroscopy of the Sun
Available online at www.sciencedirect.com Advances in Space Research 43 (2009) 1001 1006 www.elsevier.com/locate/asr TESIS experiment on EUV imaging spectroscopy of the Sun S.V. Kuzin a, *, S.A. Bogachev
Methods of surface analysis
Methods of surface analysis Nanomaterials characterisation I RNDr. Věra Vodičková, PhD. Surface of solid matter: last monoatomic layer + absorbed monolayer physical properties are effected (crystal lattice
Plumes as seen in the Ultraviolet
Plumes as seen in the Ultraviolet L. Teriaca Max Planck Institut für Sonnensystemforschung Introduction Plumes have been observed and studied since long time in white light during total eclipses (Abbot
EUV Reflectivity measurements on Acktar Sample Magic Black
Report EUV Reflectivity measurements on Acktar Sample Magic Black S. Döring, Dr. K. Mann Laser-Laboratorium Göttingen e.v. October 28, 2011 Contents 1 Introduction 3 2 Setup 3 3 Measurements 4 4 Conclusion
The Performance of the EUV Spectroscope (EXCEED) Onboard the SPRINT-A Mission
The Performance of the EUV Spectroscope (EXCEED) Onboard the SPRINT-A Mission K. Yoshioka, G. Murakami, A. Yamazaki, K. Uemizu, T. Kimura (ISAS/JAXA), I. Yoshikawa, K. Uji (Univ. Tokyo) F. Tsuchiya, and
Example: model a star using a two layer model: Radiation starts from the inner layer as blackbody radiation at temperature T in. T out.
Next, consider an optically thick source: Already shown that in the interior, radiation will be described by the Planck function. Radiation escaping from the source will be modified because the temperature
Because light behaves like a wave, we can describe it in one of two ways by its wavelength or by its frequency.
Light We can use different terms to describe light: Color Wavelength Frequency Light is composed of electromagnetic waves that travel through some medium. The properties of the medium determine how light
Recent Highlights on Solar Coronal Abundances from Hinode
Recent Highlights on Solar Coronal Abundances from Hinode David H. Brooks George Mason University Honolulu, August 10, 2015 Ignacio Ugarte-Urra/GMU Harry Warren/NRL First Ionization Potential (FIP) Effect
Observable consequences
Coronal Heating through braiding of magnetic field lines Solar eclipse, 11.8.1999, Wendy Carlos & John Kern Observable consequences 3D MHD model spectral synthesis results: Doppler shifts DEM variability
Introduction to the Diagnosis of Magnetically Confined Thermonuclear Plasma
Introduction to the Diagnosis of Magnetically Confined Thermonuclear Plasma Core diagnostics II: Bolometry and Soft X-rays J. Arturo Alonso Laboratorio Nacional de Fusión EURATOM-CIEMAT E6 P2.10 arturo.alonso@ciemat.es
Arun Kumar Awasthi (IAUWR)
Differential emission measure distribution and thermal characteristics during a B8.3 flare on July 04, 2009 Arun Kumar Awasthi Ins%tute of Astronomy University of Wroclaw, Poland E-mail: awasthi@astro.uni.wroc.pl,
Multilayer Interference Coating, Scattering, Diffraction, Reflectivity
Multilayer Interference Coating, Scattering, Diffraction, Reflectivity mλ = 2d sin θ (W/C, T. Nguyen) Normal incidence reflectivity 1..5 1 nm MgF 2 /Al Si C Pt, Au 1 ev 1 ev Wavelength 1 nm 1 nm.1 nm Multilayer
The Spectrophotometer and Atomic Spectra of Hydrogen Physics 246
The Spectrophotometer and Atomic Spectra of Hydrogen Physics 46 Introduction: When heated sufficiently, most elements emit light. With a spectrometer, the emitted light can be broken down into its various
Astronomical Techniques
Astronomers use different techniques to extract information from the light that they detect with detectors Celestial objects emit light (different wavelengths) Telescopes are used to see these distant
Review: Properties of a wave
Radiation travels as waves. Waves carry information and energy. Review: Properties of a wave wavelength (λ) crest amplitude (A) trough velocity (v) λ is a distance, so its units are m, cm, or mm, etc.
Characteristics of the Re-calculated Yohkoh/SXT Temperature Response
Solar Physics DOI: 10.1007/ - - - - Characteristics of the Re-calculated Yohkoh/SXT Temperature Response A. Takeda c Springer Abstract The temperature response functions of the Yohkoh/SXT are re-calculated
The 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
PC Laboratory Raman Spectroscopy
PC Laboratory Raman Spectroscopy Schedule: Week of September 5-9: Student presentations Week of September 19-23:Student experiments Learning goals: (1) Hands-on experience with setting up a spectrometer.