Recent solar activity. X-ray spectrophotometer SphinX. the CORONAS-PHOTON Janusz Sylwester for the SphinX team

Size: px
Start display at page:

Download "Recent solar activity. X-ray spectrophotometer SphinX. the CORONAS-PHOTON Janusz Sylwester for the SphinX team"

Transcription

1 Obserwacje strumienia promieniowania rentgenowskiego Słońca jako gwiazdy w okresie głębokiego minimum aktywności Recent solar activity as observed with X-ray spectrophotometer SphinX aboard the CORONAS-PHOTON for the SphinX team Solar Physics Division, Space Research Centre Polish Academy of Sciences, Wrocław, Kopernika 11

2 The SphinX Team SRC PAS Wrocław Mirek Kowalinski, Szymon Gburek, Marek Siarkowski, Jarek Bakala, Zbigniew Kordylewski, Piotr Podgorski, Barbara Sylwester, Anna Kepa, Witold Trzebiński P.N. Lebedev Physical Institute, Moscow Sergey Kuzin-TESIS PI, Andrei Pertsov, Sergey Bogaczev Astronomical Institute, Ondrejov Frantisek Farnik Astronomical Observatory, Palermo Fabio Reale, Alfonso Collura University College, London Ken Phillips

3 SphinX: Solar Photometer in X-rays, PI: CO RO NA Mass ~2500 kg, 8.2 GB/day S PH O TO N SRC-PAS Launched 30 Jan at 13:30 UT from Plesetsk Cosmodrome Pointing Semi-Three axis stabilised TESIS with SphinX

4 The orbit 96 min 550km, 82.5 deg. Polar orbit Life ~7 years CORONAS-F Encountered SAA ~1000 cts/s & Polar ovals ~100 cts/s 4 times/96 min

5 SphinX Polish concept, design & manufacture Measures the X-ray fluence of the Sun kev with unprecedented Time resolution ~ s Sensitivity 100 x better than GOES XRM the standard for 30+years Energy resolution 3x RHESSI (NASA)

6 The construction EUV filters (doubly aluminized Mylar) Photometer Collimators (+-2.5 deg) Three apertures D1, D2, D3 Shutter Stepper motor FFU Filters Targets D4 Electronics Front end Amptek Digital our Controller Software reprogramming Heat sink Alignment mirror Total cost of the project ~ 1 mln PLN KBN T12 grant

7 Measurement channels Photometric FFU φ: 5 mm A: 20.4mm2 8 μs Up to cts/s φ: 4 mm A: 0.50 mm2 25 μs Up to cts/s φ: 4 mm A: mm2 25 μs Up to cts/s φ: 4 mm A: 13.0 mm2 25 μs Up to cts/s FWHM: 490 ev FWHM: 290 ev FWHM: 290 ev FWHM: 290 ev Detectors (four units): 256/1024 energy bins Amptek, Peltier cooled (-50 deg C below the support T) Si PIN diodes. Detectors support plate passively cooled through the heat sink pipe to the external radiator Photon arrival time measured to within 2μs (in Time Stamping Mode)

8 How performance looks from the tests The BESSY synchrotron input spectrum (red) with overplotted response of SphinX D2 detector (black). Nominal effective areas have been used. The agreement is better than 5% in the energy band where SphinX detectors are the most sensitive. BESSY Berlin Synchrotron: - All detectors linearity: perfect (0.1% ) over kev; & dynamic range absolute response known to better than 5% against reference synchrotron source. - pile-up matrices known as measured from X-ray 4 crystal monochromator spectra obtained at 8 energies between 1.5 and 8 kev

9 GOES X class range to be extended down 10-6 W/m A = 10-8 W/m Solar X-ray flux remains at background levels: i.e. Max Millenium message S = 10-9 W/m SAA S/C night Q = W/m2 SphinX detection threshold

10 New X-ray classes We are introducing new classes of X-ray solar variability, below GOES A1.0 A = 10-8 W/m2 (present lowest) S = 10-9 W/m2 Q = W/m2 SphinX in its D1 channel is capable to observe events 100 x less intense than GOES Most of variability since the launch is observed to happen below the GOES delectability threshold

11 Solar activity: longer-term only around 80 flares,detected by GOES, among them C2.7 on 6 July 2009 and triple B on March 26, 2009 SphinX D2 record cts/s GOES detection threshold The Lowest observed level Since Launch: Long S/C day GOES 80 events, SphinX 550 events

12 Determination of absolute levels of X-ray solar luminosity E > 1 kev D1- DGI 1s E1 /E2 D1 D2

13 X-ray fluence at E > 1 kev Instrument heating Histogram of T values D2 rate D1 rate Temperature D1 rate Emission Measure Thermodynamic Measure MK Example: for data set No. 50 Te 1.71 MK [ 1.69, 1.72 ] EM 6.2 [ 5.7, 6.7] 1047 cm-3 Flux [1-15 kev] W/m2 Flux GOES [1 8 Å] W/m2

14 TESIS images (courtesy Sergey Bogaczev FIAN) :28: Å :27: Å ~ K ~1 MK

15 Longer exposure: ~18 hours Counts below 3 kev ~ 1 mln Counts above 3 kev ~ 3000 Ratio: Any coronal heating model should obey this measurement from now on

16

17 Example catalogue page D1 D2 bcg

18 Summary Two components on the lightcurves: Quasi steady X-ray intensities enhanced when AR are present The lowest quasi-steady state level, when no AR are present, is also observed in D2, this level is still fluctuating on a 5 min time scale study is in progress. Flares are seen on-top of this basal variability. Flare enhancements are being detected from amplitudes above ~ 0.05 dex. Both short and LDE types of events are present without the sunspots The Sun is the weakest X-ray star within 7 parsecs (Schmitt et al., 1995, ApJ, 450, 392) with our new estimated luminosity at LX = W 100 x less α Cen A., 47 x less previous estimates (Judge et al., 2003, ApJ, 593, 534) Luminosity in the Å is erg s-1, a value which is of interest for heating the Earth s atmosphere, much below present estimates Thermal energy content of the solar corona is erg

19 The End Please have a look at the poster Barbara Sylwester,, Marek Siarkowski Zakład Fizyki Słońca CBK PAN Wrocław: "Interpretacja widm uzyskanych za pomocą polskiego spektrofotometru SphinX"

20 Compilation of SphinX flare catalogue SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

21 Flare statistics based on SphinX catalogue interpretation (provisional) Flare amplitude vs the occurence times of events GOES detection Threshold Increasing trend is noticeable SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

22 30 April :42 A3.1 flare EIT SOHO 195 Å XRT Hinode SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

23 Spectra maximum decay E2 E1

24 Flare evolution on T-EM diagram see poster B. Sylwester et al. T EM ThM = T * sqrt(em)

25 Diagnostic Diagram Jakimiec, J.; Sylwester, B. ; Sylwester, J.; Serio, S.; Peres, G.; Reale, F. 1992A&A From HXIS A eh C L Palermo-Harvard Code Peres et al., 1982 A eh C L Jakimiec, J.; Sylwester, B.; Sylwester, J.; Mewe, R.; Peres, G., 1986AdSpR J SS RTV: 2 Log T ½ Log EM = ½ Log(L/2A)

26 Diagnostic diagram based on GOES Sylwester, J.; Sylwester, B.; Phillips, K. J. H.; Kepa, A. g n i n ar W

27 06 June 2009 B2.6 flare TESIS 171 Å XRT Hinode SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

28 Spectra maximum decay E2 E1 SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

29 Flare evolution on T-EM diagram see poster B. Sylwester et al. T EM ThM = T * sqrt(em)

30 Conclusions SphinX will provide flare flags to Coronas (testing algorithms in orbit) Sphinx measurements allow To See solar X-ray variability from the bottom level up to X20 To Determine absolute fluxes above 1 kev, each few s (also GOES in standard bands) To Study photon arrival times statistics (needs some more work on the instrument operation) To Study small flare statistics Will supplement RHESSI spectra towards lower energies Will provide the most exhaustive flare catalogue SOLAR CORONAL LOOPS WORKSHOP IV, Wednesday, July 1, 2009 : Activity - SphinX

SphinX:A Fast Solar Photometer in X-rays. J. Sylwester 1,, S. Kuzin 2, Yu. D. Kotov 3, F. Farnik 4 & F. Reale 5

SphinX:A Fast Solar Photometer in X-rays. J. Sylwester 1,, S. Kuzin 2, Yu. D. Kotov 3, F. Farnik 4 & F. Reale 5 J. Astrophys. Astr. (2008) 29, 339 343 SphinX:A Fast Solar Photometer in X-rays J. Sylwester 1,, S. Kuzin 2, Yu. D. Kotov 3, F. Farnik 4 & F. Reale 5 1 Space Research Center, Polish Academy of Sciences,

More information

New instruments under development at Wrocław SPD, SRC. RESPECT Rosja, FIAN SphinX-NG, GSFC

New instruments under development at Wrocław SPD, SRC. RESPECT Rosja, FIAN SphinX-NG, GSFC New instruments under development at Wrocław SPD, SRC RESPECT Rosja, FIAN SphinX-NG, GSFC SphinX heritage (PIN diode detectors) There is a lower limit for solar X-ray flux of the Sun in the energy range

More information

CHROMOSPHERIC DYNAMICS FROM RHESSI AND RESIK DATA

CHROMOSPHERIC DYNAMICS FROM RHESSI AND RESIK DATA CHROMOSPHERIC DYNAMICS FROM RHESSI AND RESIK DATA T. Mrozek 1,2, S. Kołomański 2,B. Sylwester 1, A. Kępa 1, J. Sylwester 1, S. Gburek 1, M. Siarkowski 1, M. Gryciuk 1, M. Stęślicki 1 1 Solar Physics Division,

More information

Investigations of Physical Processes in Solar Flare Plasma on the Basis of RESIK Spectrometer Observations

Investigations of Physical Processes in Solar Flare Plasma on the Basis of RESIK Spectrometer Observations Investigations of Physical Processes in Solar Flare Plasma on the Basis of RESIK Spectrometer Observations Z Kordylewski, J Sylwester, B Sylwester, A Kȩpa, M Kowaliński, and W Trzebiński X-ray spectroscopy

More information

Resolving physical line profiles from Bragg X-ray spectra using Withbroe-Sylwester deconvolution

Resolving physical line profiles from Bragg X-ray spectra using Withbroe-Sylwester deconvolution Resolving physical line profiles from Bragg X-ray spectra using Withbroe-Sylwester deconvolution Janusz Sylwester Ż. Szaforz, M. Stęślicki, B. Sylwester, PL K.J.H. Phillips, UK Outline The problem & rationale

More information

This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00

This paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00 Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June

More information

XRT Detection of Hot Plasma in Active Regions and Nanoflare Heating

XRT Detection of Hot Plasma in Active Regions and Nanoflare Heating XRT Detection of Hot Plasma in Active Regions and Nanoflare Heating Dipartimento di Scienze Fisiche & Astronomiche, Università di Palermo, & INAF/Osservatorio Astronomico di Palermo, Italy reale@astropa.unipa.it

More information

Heating diagnostics with MHD waves

Heating diagnostics with MHD waves Heating diagnostics with MHD waves R. Erdélyi & Y. Taroyan Robertus@sheffield.ac.uk SP 2 RC, Department of Applied Mathematics, The University of Sheffield (UK) The solar corona 1860s coronium discovered

More information

Observing the Sun from space: Highlights from Yohkoh, SOHO, TRACE, RHESSI. H.S. Hudson Space Sciences Lab University of California, Berkeley

Observing the Sun from space: Highlights from Yohkoh, SOHO, TRACE, RHESSI. H.S. Hudson Space Sciences Lab University of California, Berkeley Observing the Sun from space: Highlights from Yohkoh, SOHO, TRACE, RHESSI H.S. Hudson Space Sciences Lab University of California, Berkeley SUMMARY OF LECTURE I. Overview of the Sun 2. Observational technique

More information

Mars Atmosphere and Volatile EvolutioN (MAVEN) Mission

Mars Atmosphere and Volatile EvolutioN (MAVEN) Mission Mars Atmosphere and Volatile EvolutioN (MAVEN) Mission MAVEN Science Community Workshop December 2, 2012 Particles and Fields Package Solar Energetic Particle Instrument (SEP) Davin Larson and the SEP

More information

BB-18 Black Body High Vacuum System Technical Description

BB-18 Black Body High Vacuum System Technical Description BB-18 Black Body High Vacuum System Technical Description The BB-18 Black Body is versatile and is programmed for use as a fixed cold target at 80 K or variable target, at 80 K- 350 K no extra cost. The

More information

Development of the Extreme Ultraviolet Spectrometer: EXCEED

Development of the Extreme Ultraviolet Spectrometer: EXCEED Development of the Extreme Ultraviolet Spectrometer: EXCEED Go Murakami*, Kazuo Yoshioka, Atsushi Yamazaki, Tomoki Kimura Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency

More information

SPIRIT/CORONAS-F experiment

SPIRIT/CORONAS-F experiment SPIRIT/CORONAS-F experiment S.V. Kuzin, V.A. Slemzin, A.M. Urnov P.N. Lebedev Physics Institute of RAS Leninsky pr., 53, Moscow, Russia 1. Description of the SPIRIT instrument Spectral bands Optical design

More information

Solar atmosphere. Solar activity and solar wind. Reading for this week: Chap. 6.2, 6.3, 6.5, 6.7 Homework #2 (posted on website) due Oct.

Solar atmosphere. Solar activity and solar wind. Reading for this week: Chap. 6.2, 6.3, 6.5, 6.7 Homework #2 (posted on website) due Oct. Solar activity and solar wind Solar atmosphere Reading for this week: Chap. 6.2, 6.3, 6.5, 6.7 Homework #2 (posted on website) due Oct. 17 Photosphere - visible surface of sun. Only ~100 km thick. Features

More information

Progress Towards the Solar Dynamics Observatory

Progress Towards the Solar Dynamics Observatory Progress Towards the Solar Dynamics Observatory Barbara J. Thompson SDO Project Scientist W. Dean Pesnell SDO Assistant Project Scientist Page 1 SDO OVERVIEW Mission Science Objectives The primary goal

More information

Solar Flare Composition and Thermodynamics from RESIK X-ray Spectra

Solar Flare Composition and Thermodynamics from RESIK X-ray Spectra Solar Flare Composition and Thermodynamics from RESIK X-ray Spectra B. Sylwester 1 and J. Sylwester 1 1 Space Research Center, Polish Academy of Sciences, Kopernika 11, 51-622 Wrocław, Poland arxiv:1404.5775v2

More information

Use the following image to answer the next question. 1. Which of the following rows identifies the electrical charge on A and B shown above?

Use the following image to answer the next question. 1. Which of the following rows identifies the electrical charge on A and B shown above? Old Science 30 Physics Practice Test A on Fields and EMR Test Solutions on the Portal Site Use the following image to answer the next question 1. Which of the following rows identifies the electrical charge

More information

Solar Irradiance Variability Observed During Solar Cycle 23

Solar Irradiance Variability Observed During Solar Cycle 23 Solar Irradiance Variability Observed During Solar Cycle 23 Introduction Solar Cycle Results for Climate Change Solar Cycle Results for Space Weather Tom Woods LASP / University

More information

Solar Ast ro p h y s ics

Solar Ast ro p h y s ics Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3

More information

Satellite Measurements of Solar Spectral Irradiance

Satellite Measurements of Solar Spectral Irradiance Satellite Measurements of Solar Spectral Irradiance LASP University of Colorado tom.woods@lasp.colorado.edu March 2006 1 Talk Outline Motivation for Solar Spectral Irradiance solar energy input climate

More information

!"#$%&'%!%#'$(&$%)*'%+&",-.!(&#$#/%01&,2&!$.%)$%!& &!,-#'& "(1!.$!&/.3.!.,)& & 4',$5#4& & & '%",'*&2,'&6789& &

!#$%&'%!%#'$(&$%)*'%+&,-.!(&#$#/%01&,2&!$.%)$%!& &!,-#'& (1!.$!&/.3.!.,)& & 4',$5#4& & & '%,'*&2,'&6789& & !!!"#$%'%!%#'$($%)*'%+",-.!(#$#/%01,2!$.%)$%!!,-#' "(1!.$!/.3.!.,) 4',$5#4 '%",'*2,'6789!! :;?!@ABC>DCE 2CFE=;E@678G H;>CIJ

More information

An Introduction to the MTG-IRS Mission

An Introduction to the MTG-IRS Mission An Introduction to the MTG-IRS Mission Stefano Gigli, EUMETSAT IRS-NWC Workshop, Eumetsat HQ, 25-0713 Summary 1. Products and Performance 2. Design Overview 3. L1 Data Organisation 2 Part 1 1. Products

More information

High resolution images obtained with Solar Optical Telescope on Hinode. SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ)

High resolution images obtained with Solar Optical Telescope on Hinode. SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ) High resolution images obtained with Solar Optical Telescope on Hinode SOLAR-B Project Office National Astronomical Observatory of Japan (NAOJ) Temperature stratification of solar atmosphere G-band Ca

More information

Chapter 2: Solar Radiation and Seasons

Chapter 2: Solar Radiation and Seasons Chapter 2: Solar Radiation and Seasons Spectrum of Radiation Intensity and Peak Wavelength of Radiation Solar (shortwave) Radiation Terrestrial (longwave) Radiations How to Change Air Temperature? Add

More information

Atomic Physics Measurements in Support of X-ray Astronomy

Atomic Physics Measurements in Support of X-ray Astronomy Atomic Physics Measurements in Support of X-ray Astronomy Your LDRD Representative Graphic Here (Fit in this rectangle, no caption) Oct 27, 2010 Gatlinburg P. Beiersdorfer G. Brown LLNL M. Frankel LLNL*

More information

PTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY

PTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY PTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY Due Date: start of class 2/6/2007 5 pts extra credit if turned in before 9:00AM (early!) (To get the extra credit, the assignment must

More information

Some Basic Principles from Astronomy

Some Basic Principles from Astronomy Some Basic Principles from Astronomy The Big Question One of the most difficult things in every physics class you will ever take is putting what you are learning in context what is this good for? how do

More information

Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation

Light as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered

More information

Energy savings in commercial refrigeration. Low pressure control

Energy savings in commercial refrigeration. Low pressure control Energy savings in commercial refrigeration equipment : Low pressure control August 2011/White paper by Christophe Borlein AFF and l IIF-IIR member Make the most of your energy Summary Executive summary

More information

SOLSPEC MEASUREMENT OF THE SOLAR ABSOLUTE SPECTRAL IRRADIANCE FROM 165 to 2900 nm ON BOARD THE INTERNATIONAL SPACE STATION

SOLSPEC MEASUREMENT OF THE SOLAR ABSOLUTE SPECTRAL IRRADIANCE FROM 165 to 2900 nm ON BOARD THE INTERNATIONAL SPACE STATION SOLSPEC MEASUREMENT OF THE SOLAR ABSOLUTE SPECTRAL IRRADIANCE FROM 165 to 2900 nm ON BOARD THE INTERNATIONAL SPACE STATION G. Thuillier1, D. Bolsee2 1 LATMOS-CNRS, France 2 Institut d Aéronomie Spatiale

More information

Science Standard 4 Earth in Space Grade Level Expectations

Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal

More information

Janet Machol NOAA National Geophysical Data Center University of Colorado CIRES. Rodney Viereck NOAA Space Weather Prediction Center

Janet Machol NOAA National Geophysical Data Center University of Colorado CIRES. Rodney Viereck NOAA Space Weather Prediction Center Janet Machol NOAA National Geophysical Data Center University of Colorado CIRES Rodney Viereck NOAA Space Weather Prediction Center Andrew Jones University of Colorado LASP Inter-Calibration and Degradation

More information

Space Weather: Forecasting & Impacts on Critical Infrastructure

Space Weather: Forecasting & Impacts on Critical Infrastructure Space Weather: Forecasting & Impacts on Critical Infrastructure Dr. Genene Fisher Senior Advisor for Space Weather National Weather Service AMS Washington Forum 12 April 2012 Outline Solar Activity Update

More information

Take away concepts. What is Energy? Solar Energy. EM Radiation. Properties of waves. Solar Radiation Emission and Absorption

Take away concepts. What is Energy? Solar Energy. EM Radiation. Properties of waves. Solar Radiation Emission and Absorption Take away concepts Solar Radiation Emission and Absorption 1. 2. 3. 4. 5. 6. Conservation of energy. Black body radiation principle Emission wavelength and temperature (Wein s Law). Radiation vs. distance

More information

ILX Lightwave Corporation www.ilxlightwave.com

ILX Lightwave Corporation www.ilxlightwave.com # 14 Optimizing TEC Current Optimizing TEC Drive Current This Application Note discusses methods for optimizing the TEC drive current for optimum operation in heating and cooling applications. BACKGROUND

More information

Solar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation

Solar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics

More information

CSSAR Space Science Cooperation

CSSAR Space Science Cooperation CSSAR Space Science Cooperation WANG Shuzhi Center for Space Science and Applied Research Chinese Academy of Science(CSSAR) Table of Contents Brief History of CSSAR International Cooperation CAS Strategic

More information

From Nobeyama to ALMA

From Nobeyama to ALMA Highlights of Nobeyama Solar Results: From Nobeyama to ALMA Kiyoto Shibasaki Nobeyama Solar Radio Observatory 2013/1/15 Solar ALMA WS @ Glasgow 1 Outline Short history Solar physics with radio observations

More information

Solar Active Region:Heating and Dynamics L.K. Harra-Murnion and S.A. Matthews Mullard Space Science Laboratory, University College London, Holmbury St. Mary, Dorking, Surrey RH5 6NT, U.K. H. Hara and K.

More information

Statistical Distributions in Astronomy

Statistical Distributions in Astronomy Data Mining In Modern Astronomy Sky Surveys: Statistical Distributions in Astronomy Ching-Wa Yip cwyip@pha.jhu.edu; Bloomberg 518 From Data to Information We don t just want data. We want information from

More information

Characteristic curves of a solar cell

Characteristic curves of a solar cell Related Topics Semi-conductor, p-n junction, energy-band diagram, Fermi characteristic energy level, diffusion potential, internal resistance, efficiency, photo-conductive effect, acceptors, donors, valence

More information

Corso di Fisica Te T cnica Ambientale Solar Radiation

Corso di Fisica Te T cnica Ambientale Solar Radiation Solar Radiation Solar radiation i The Sun The Sun is the primary natural energy source for our planet. It has a diameter D = 1.39x10 6 km and a mass M = 1.989x10 30 kg and it is constituted by 1/3 of He

More information

Evidence in White Light of Post-CME Current Sheets Mostly Observational

Evidence in White Light of Post-CME Current Sheets Mostly Observational Evidence in White Light of Post-CME Current Sheets Mostly Observational David Webb ISR, Boston College OUTLINE Review previous results of SMM & LASCO WL rays trailing CMEs - Lifetimes, lengths (heights)

More information

CBERS Program Update Jacie 2011. Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com

CBERS Program Update Jacie 2011. Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com CBERS Program Update Jacie 2011 Frederico dos Santos Liporace AMS Kepler liporace@amskepler.com Overview CBERS 3 and 4 characteristics Differences from previous CBERS satellites (CBERS 1/2/2B) Geometric

More information

The Sun. Solar radiation (Sun Earth-Relationships) The Sun. The Sun. Our Sun

The Sun. Solar radiation (Sun Earth-Relationships) The Sun. The Sun. Our Sun The Sun Solar Factoids (I) The sun, a medium-size star in the milky way galaxy, consisting of about 300 billion stars. (Sun Earth-Relationships) A gaseous sphere of radius about 695 500 km (about 109 times

More information

# 2. Selecting and Using Thermistors for Temperature Control

# 2. Selecting and Using Thermistors for Temperature Control # 2 Selecting and Using Thermistors for Temperature Control Selecting and Using Thermistors for Temperature Control Thermally sensitive resistors (thermistors) are used widely in laser diode and detector

More information

CHAPTER 2 Energy and Earth

CHAPTER 2 Energy and Earth CHAPTER 2 Energy and Earth This chapter is concerned with the nature of energy and how it interacts with Earth. At this stage we are looking at energy in an abstract form though relate it to how it affect

More information

Laue lens for Nuclear Medicine

Laue lens for Nuclear Medicine Laue lens for Nuclear Medicine PhD in Physics Gianfranco Paternò Ferrara, 6-11-013 Supervisor: prof. Vincenzo Guidi Sensors and Semiconductors Lab, Department of Physics and Earth Science, University of

More information

Examples of Uniform EM Plane Waves

Examples of Uniform EM Plane Waves Examples of Uniform EM Plane Waves Outline Reminder of Wave Equation Reminder of Relation Between E & H Energy Transported by EM Waves (Poynting Vector) Examples of Energy Transport by EM Waves 1 Coupling

More information

2 Absorbing Solar Energy

2 Absorbing Solar Energy 2 Absorbing Solar Energy 2.1 Air Mass and the Solar Spectrum Now that we have introduced the solar cell, it is time to introduce the source of the energy the sun. The sun has many properties that could

More information

Main sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya

Main sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya Main sequence stars Haris Ðapo 1 Akdeniz University, Antalya Antalya Lecture 3. Haris Ðapo (Akdeniz University) Main sequence stars Main sequence stars 1 / 22 Outline 1 Introduction 2 Hydrogen burning

More information

Lecture 14. Introduction to the Sun

Lecture 14. Introduction to the Sun Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum

More information

16 th IOCCG Committee annual meeting. Plymouth, UK 15 17 February 2011. mission: Present status and near future

16 th IOCCG Committee annual meeting. Plymouth, UK 15 17 February 2011. mission: Present status and near future 16 th IOCCG Committee annual meeting Plymouth, UK 15 17 February 2011 The Meteor 3M Mt satellite mission: Present status and near future plans MISSION AIMS Satellites of the series METEOR M M are purposed

More information

Status of the XIS Orbital Calibration and Softwares

Status of the XIS Orbital Calibration and Softwares Status of the XIS Orbital Calibration and Softwares K. Hayashida,, N. Tawa,, M. Nagai, H. Nakajima, M. Uchino, N. Anabuki,, S. Katsuda,, H. Uchida, H. Tsunemi (Osaka Univ.), H. Matsumoto,, H. Mori, H.

More information

Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh

Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How

More information

Department of Engineering Enzo Ferrari University of Modena and Reggio Emilia

Department of Engineering Enzo Ferrari University of Modena and Reggio Emilia Department of Engineering Enzo Ferrari University of Modena and Reggio Emilia Object: Measurement of solar reflectance, thermal emittance and Solar Reflectance Index Report Reference person: Alberto Muscio

More information

Passive Millimeter-Wave Imaging and Potential Applications in Homeland Security and Aeronautics

Passive Millimeter-Wave Imaging and Potential Applications in Homeland Security and Aeronautics Passive Millimeter-Wave Imaging and Potential Applications in Homeland Security and Aeronautics Magdy Attia, Ph.D. James B. Duke Distinguished Professor Chair, Computer Science & Engineering Department

More information

Solar Flux and Flux Density. Lecture 3: Global Energy Cycle. Solar Energy Incident On the Earth. Solar Flux Density Reaching Earth

Solar Flux and Flux Density. Lecture 3: Global Energy Cycle. Solar Energy Incident On the Earth. Solar Flux Density Reaching Earth Lecture 3: Global Energy Cycle Solar Flux and Flux Density Planetary energy balance Greenhouse Effect Vertical energy balance Latitudinal energy balance Seasonal and diurnal cycles Solar Luminosity (L)

More information

Activitity (of a radioisotope): The number of nuclei in a sample undergoing radioactive decay in each second. It is commonly expressed in curies

Activitity (of a radioisotope): The number of nuclei in a sample undergoing radioactive decay in each second. It is commonly expressed in curies Activitity (of a radioisotope): The number of nuclei in a sample undergoing radioactive decay in each second. It is commonly expressed in curies (Ci), where 1 Ci = 3.7x10 10 disintegrations per second.

More information

PHSC 3033: Meteorology Seasons

PHSC 3033: Meteorology Seasons PHSC 3033: Meteorology Seasons Changing Aspect Angle Direct Sunlight is more intense and concentrated. Solar Incidence Angle is Latitude and Time/Date Dependent Daily and Seasonal Variation Zenith There

More information

The VHE future. A. Giuliani

The VHE future. A. Giuliani The VHE future A. Giuliani 1 The Cherenkov Telescope Array Low energy Medium energy High energy 4.5o FoV 7o FoV 10o FoV 2000 pixels 2000 pixels 2000 pixels ~ 0.1 ~ 0.18 ~ 0.2-0.3 The Cherenkov Telescope

More information

A Quick primer on synchrotron radiation: How would an MBA source change my x-ray beam. Jonathan Lang Advanced Photon Source

A Quick primer on synchrotron radiation: How would an MBA source change my x-ray beam. Jonathan Lang Advanced Photon Source A Quick primer on synchrotron radiation: How would an MBA source change my x-ray beam Jonathan Lang Advanced Photon Source APS Upgrade - MBA Lattice ε ο = 3100 pm ε ο = 80 pm What is emi7ance? I don t

More information

How To Understand Light And Color

How To Understand Light And Color PRACTICE EXAM IV P202 SPRING 2004 1. In two separate double slit experiments, an interference pattern is observed on a screen. In the first experiment, violet light (λ = 754 nm) is used and a second-order

More information

The Physics of Energy sources Renewable sources of energy. Solar Energy

The Physics of Energy sources Renewable sources of energy. Solar Energy The Physics of Energy sources Renewable sources of energy Solar Energy B. Maffei Bruno.maffei@manchester.ac.uk Renewable sources 1 Solar power! There are basically two ways of using directly the radiative

More information

Fermi LAT and GBM Data Access, File Structure and the Standard Tools. Fermi Solar Analysis Workshop GSFC, August 2012 Elizabeth Ferrara - FSSC 1

Fermi LAT and GBM Data Access, File Structure and the Standard Tools. Fermi Solar Analysis Workshop GSFC, August 2012 Elizabeth Ferrara - FSSC 1 Fermi LAT and GBM Data Access, File Structure and the Standard Tools Fermi Solar Analysis Workshop GSFC, August 2012 Elizabeth Ferrara - FSSC 1 Fermi Science Support Center Home Current News, FAQ, Helpdesk

More information

STUDY GUIDE: Earth Sun Moon

STUDY GUIDE: Earth Sun Moon The Universe is thought to consist of trillions of galaxies. Our galaxy, the Milky Way, has billions of stars. One of those stars is our Sun. Our solar system consists of the Sun at the center, and all

More information

Introduction to Astronomy. Lecture 4: Our star, the Sun

Introduction to Astronomy. Lecture 4: Our star, the Sun Introduction to Astronomy Lecture 4: Our star, the Sun 1 Sun Facts Age = 4.6 x 10 9 years Mean Radius = 7.0x10 5 km = 1.1x10 2 R = 1R Volume = 1.4x10 18 km 3 = 1.3x10 6 R = 1V Mass = 2x10 30 kg = 3.3x10

More information

The Sun: Our nearest star

The Sun: Our nearest star The Sun: Our nearest star Property Surface T Central T Luminosity Mass Lifetime (ms) Value 5500K 15x10 6 K 2 x 10 33 ergs 4 x 10 33 grams 10 billion years Solar Structure Build a model and find the central

More information

DS 600. A contact free flux gate based current measurement sensor 600A rms

DS 600. A contact free flux gate based current measurement sensor 600A rms DS 600 A contact free flux gate based current measurement sensor 600A rms DS 600 is member of the small housing sensor family. The family includes a 200A and a 600A version. 600A rms - 900A peak Maximum

More information

Solar Forcing of Electron and Ion Auroral Inputs

Solar Forcing of Electron and Ion Auroral Inputs Solar Forcing of Electron and Ion Auroral Inputs Barbara A. Emery (NCAR), Ian G. Richardson (GSFC), David S. Evans (NOAA), Frederick J. Rich (LL/MIT), Gordon Wilson (AFRL), Sarah Gibson (NCAR), Giuliana

More information

Observing the Sun NEVER LOOK DIRECTLY AT THE SUN!!! Image taken from the SOHO web-site http://sohowww.nascom.nasa.gov/gallery/solarcorona/uvc003.

Observing the Sun NEVER LOOK DIRECTLY AT THE SUN!!! Image taken from the SOHO web-site http://sohowww.nascom.nasa.gov/gallery/solarcorona/uvc003. name Observing the Sun NEVER LOOK DRECTLY AT THE SUN!!! mage taken from the SOHO web-site http://sohowww.nascom.nasa.gov/gallery/solarcorona/uvc003.html Explanation: The Sun is a pretty active star. You

More information

8.1 Radio Emission from Solar System objects

8.1 Radio Emission from Solar System objects 8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio

More information

Teaching Time: One-to-two 50-minute periods

Teaching Time: One-to-two 50-minute periods Lesson Summary Students create a planet using a computer game and change features of the planet to increase or decrease the planet s temperature. Students will explore some of the same principles scientists

More information

The accurate calibration of all detectors is crucial for the subsequent data

The accurate calibration of all detectors is crucial for the subsequent data Chapter 4 Calibration The accurate calibration of all detectors is crucial for the subsequent data analysis. The stability of the gain and offset for energy and time calibration of all detectors involved

More information

Using Photometric Data to Derive an HR Diagram for a Star Cluster

Using Photometric Data to Derive an HR Diagram for a Star Cluster Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and

More information

Blackbody radiation. Main Laws. Brightness temperature. 1. Concepts of a blackbody and thermodynamical equilibrium.

Blackbody radiation. Main Laws. Brightness temperature. 1. Concepts of a blackbody and thermodynamical equilibrium. Lecture 4 lackbody radiation. Main Laws. rightness temperature. Objectives: 1. Concepts of a blackbody, thermodynamical equilibrium, and local thermodynamical equilibrium.. Main laws: lackbody emission:

More information

Gamma and X-Ray Detection

Gamma and X-Ray Detection Gamma and X-Ray Detection DETECTOR OVERVIEW The kinds of detectors commonly used can be categorized as: a. Gas-filled Detectors b. Scintillation Detectors c. Semiconductor Detectors The choice of a particular

More information

Ionospheric Research with the LOFAR Telescope

Ionospheric Research with the LOFAR Telescope Ionospheric Research with the LOFAR Telescope Leszek P. Błaszkiewicz Faculty of Mathematics and Computer Science, UWM Olsztyn LOFAR - The LOw Frequency ARray The LOFAR interferometer consist of a large

More information

Counting Sunspots. Parent Prompts: Are there years with lots of sunspots? Are there years with very few sunspots?

Counting Sunspots. Parent Prompts: Are there years with lots of sunspots? Are there years with very few sunspots? Counting are magnetic storms on the Sun these dark areas are a little cooler than the rest of the Sun s atmosphere. They can be easily seen when the Sun s image is projected onto a white surface, using

More information

Vicot Solar Air Conditioning. V i c o t A i r C o n d i t i o n i n g C o., l t d Tel: 86-531-8235 5576 Fax: 86-531-82357911 Http://www.vicot.com.

Vicot Solar Air Conditioning. V i c o t A i r C o n d i t i o n i n g C o., l t d Tel: 86-531-8235 5576 Fax: 86-531-82357911 Http://www.vicot.com. Vicot Solar Air Conditioning V i c o t A i r C o n d i t i o n i n g C o., l t d Tel: 86-531-8235 5576 Fax: 86-531-82357911 Http://www.vicot.com.cn Cooling, heating, and domestic hot water. Return on investment

More information

Ay 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable

Ay 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater

More information

Radiation Transfer in Environmental Science

Radiation Transfer in Environmental Science Radiation Transfer in Environmental Science with emphasis on aquatic and vegetation canopy media Autumn 2008 Prof. Emmanuel Boss, Dr. Eyal Rotenberg Introduction Radiation in Environmental sciences Most

More information

SECTION 1: REQUIREMENTS FOR CERTIFICATES OF COMPLIANCE FOR CLASSES OF RADIATION APPARATUS

SECTION 1: REQUIREMENTS FOR CERTIFICATES OF COMPLIANCE FOR CLASSES OF RADIATION APPARATUS Department of Health and Human Services Population Health Radiation Protection Act 2005 Section 17 CERTIFICATE OF COMPLIANCE: STANDARD FOR RADIATION APPARATUS - X-RAY MEDICAL DIAGNOSTIC (MOBILE RADIOGRAPHY)

More information

HP 70950B OPTICAL SPECTRUM ANALYZER

HP 70950B OPTICAL SPECTRUM ANALYZER HP 71450B, 71451B, and 71452B Optical Spectrum Analyzers Technical Specifications Spectral Measurements from 600 to 1700 nm HP 70950B OPTICAL SPECTRUM ANALYZER OPTICAL INPUT The HP 71450B, 71451B, and

More information

Spectra of pyroelectric X-ray generator

Spectra of pyroelectric X-ray generator Abstract Spectra of pyroelectric X-ray generator Nagaychenko V.I., Sanin V.M., Yegorov A.M., Shchagin A.V. Kharkov Institute of Physics and Technology, Kharkov 6118, Ukraine The construction of X-ray generator

More information

Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board

Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board Yukikatsu Terada (Saitama Univ, Japan), on behalf of the Astro-H Software Calibration board SKIP (Rob Introduction) The sixth series of the Japanese X-ray satellite. Collaboration with JAXA, NASA, and

More information

Amptek Application Note XRF-1: XRF Spectra and Spectra Analysis Software By R.Redus, Chief Scientist, Amptek Inc, 2008.

Amptek Application Note XRF-1: XRF Spectra and Spectra Analysis Software By R.Redus, Chief Scientist, Amptek Inc, 2008. Amptek Application Note XRF-1: XRF Spectra and Spectra Analysis Software By R.Redus, Chief Scientist, Amptek Inc, 2008. X-Ray Fluorescence (XRF) is a very simple analytical technique: X-rays excite atoms

More information

Remote Level Monitoring Unit

Remote Level Monitoring Unit Remote Level Monitoring Unit SPECIFICATIONS LASER MEASUREMENT Type InGasAs Laser Diode Wavelength 905 nm Beam Divergence 2.3 x 0.2 mrad (typical) Passive Range 0.5m to 150m Range to Reflective Target 0.5m

More information

Solar Storms and Northern lights - how to predict Space Weather and the Aurora

Solar Storms and Northern lights - how to predict Space Weather and the Aurora Solar Storms and Northern lights - how to predict Space Weather and the Aurora Pål Brekke Norwegian Space Centre/UNIS Pål Brekke torsdag 12. mars 15 Fleet of satellites watching the Sun Stereo SDO SOHO

More information

WELCOME to Aurorae In the Solar System. J.E. Klemaszewski

WELCOME to Aurorae In the Solar System. J.E. Klemaszewski WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets

More information

2. Orbits. FER-Zagreb, Satellite communication systems 2011/12

2. Orbits. FER-Zagreb, Satellite communication systems 2011/12 2. Orbits Topics Orbit types Kepler and Newton laws Coverage area Influence of Earth 1 Orbit types According to inclination angle Equatorial Polar Inclinational orbit According to shape Circular orbit

More information

Fig.1. The DAWN spacecraft

Fig.1. The DAWN spacecraft Introduction Optical calibration of the DAWN framing cameras G. Abraham,G. Kovacs, B. Nagy Department of Mechatronics, Optics and Engineering Informatics Budapest University of Technology and Economics

More information

Transmissive Optical Sensor with Phototransistor Output

Transmissive Optical Sensor with Phototransistor Output TCST11. up to TCST23. Transmissive Optical Sensor with Phototransistor Output Description This device has a compact construction where the emitting-light sources and the detectors are located face-to-face

More information

Solar Wind: Theory. Parker s solar wind theory

Solar Wind: Theory. Parker s solar wind theory Solar Wind: Theory The supersonic outflow of electrically charged particles, mainly electrons and protons from the solar CORONA, is called the SOLAR WIND. The solar wind was described theoretically by

More information

Detecting and measuring faint point sources with a CCD

Detecting and measuring faint point sources with a CCD Detecting and measuring faint point sources with a CCD Herbert Raab a,b a Astronomical ociety of Linz, ternwarteweg 5, A-400 Linz, Austria b Herbert Raab, chönbergstr. 3/1, A-400 Linz, Austria; herbert.raab@utanet.at

More information

MY FIRST STEPS IN SLIT SPECTROSCOPY

MY FIRST STEPS IN SLIT SPECTROSCOPY MY FIRST STEPS IN SLIT SPECTROSCOPY Andrew Wilson BAAVSS Spectroscopy Workshop Norman Lockyer Observatory October 2015 Overview My choice of spectrograph, camera and telescope Getting started and basic

More information

Physics Notes Class 11 CHAPTER 2 UNITS AND MEASUREMENTS

Physics Notes Class 11 CHAPTER 2 UNITS AND MEASUREMENTS 1 P a g e Physics Notes Class 11 CHAPTER 2 UNITS AND MEASUREMENTS The comparison of any physical quantity with its standard unit is called measurement. Physical Quantities All the quantities in terms of

More information

Cosmic Structure Formation and Dynamics: Cosmological N-body Simulations of Galaxy Formation and Magnetohydrodynamic Simulations of Solar Atmosphere

Cosmic Structure Formation and Dynamics: Cosmological N-body Simulations of Galaxy Formation and Magnetohydrodynamic Simulations of Solar Atmosphere Chapter 3 Epoch Making Simulation Cosmic Structure Formation and Dynamics: Cosmological N-body Simulations of Galaxy Formation and Magnetohydrodynamic Simulations of Solar Atmosphere Project Representative

More information

How does snow melt? Principles of snow melt. Energy balance. GEO4430 snow hydrology 21.03.2006. Energy flux onto a unit surface:

How does snow melt? Principles of snow melt. Energy balance. GEO4430 snow hydrology 21.03.2006. Energy flux onto a unit surface: Principles of snow melt How does snow melt? We need energy to melt snow/ ice. GEO443 snow hydrology 21.3.26 E = m L h we s K = ρ h = w w we f E ρ L L f f Thomas V. Schuler t.v.schuler@geo.uio.no E energy

More information

V6 AIRS Spectral Calibra2on

V6 AIRS Spectral Calibra2on V6 AIRS Spectral Calibra2on Evan Manning Bob Deen Yibo Jiang George Aumann Denis EllioA Jet Propulsion Laboratory California Ins2tute of Technology 5/4/09 1 Spectral Calibra2on Primer AIRS measures radiance

More information