Irradiance Variation at Solar Minimum: Real or Instrumental? David Rust, JHU/APL Space Physics Group A Cooperative Research Project for the International.

Slides:

Advertisements

Similar presentations

“Adelaide May Have the Dubious Distinction of Being the First Industrialized City to Live in a Constant State of Water Shortage” (National Geographic Magazine,

Advertisements

Chapter 8 The Sun – Our Star.

1 Fingerprints in Sunlight Understanding Spectroscopy Stanford University Solar Center.

The Sun’s Dynamic Atmosphere Lecture 15. Guiding Questions 1.What is the temperature and density structure of the Sun’s atmosphere? Does the atmosphere.

RADIATIVE PROPERTIES OF REAL MATERIALS Electromagnetic Theory: ▪ ideal, optically smooth surface ▪ valid for spectral range larger than visible Real Materials:

SOLIS: Status and results Alexei A. Pevtsov (National Solar Observatory, USA)

SOLAR IRRADIANCE VARIABILITY OF RELEVANCE FOR CLIMATE STUDIES N.A. Krivova.

We are in a Revolutionary Period in our Understanding of the Sun because of New Data 10 Years of YOHKOH X-Ray Images 12 Years of SOHO Magnetograms, Dopplergrams,

1 G. Cessateur, T. Dudok de Wit, M. Kretzschmar, L. Vieira LPC2E, University of Orléans, France J. Lilensten LPG, University of Grenoble, France New Models.

The EUV spectral irradiance of the Sun from minimum to maximum Giulio Del Zanna Department of Space and Climate Physics University College London Vincenzo.

High-latitude activity and its relationship to the mid-latitude solar activity. Elena E. Benevolenskaya & J. Todd Hoeksema Stanford University Abstract.

Remarkable Low Temperature Emission of the 4 November 2003 Limb Flare J. Leibacher, J. Harvey, GONG Team (NSO), G. Kopp (CU/LASP), H. Hudson (UCB/SSL)

HMI – Synoptic Data Sets HMI Team Meeting Jan. 26, 2005 Stanford, CA.

Measuring the shape of the Sun H.S. Hudson, M.D. Fivian & H.J. Zahid Space Sciences Lab, UC Berkeley.

SDO Project Science Team 1 The Science of SDO. SDO Project Science Team 2 Sensing the Sun from Space  High-resolution Spectroscopy for Helioseismology.

Temperature Minimum Region between the Minimum-Activity Epochs and W. Livingston and E. Avrett AGU Fall Meeting, 2003.

1.B – Solar Dynamo 1.C – Global Circulation 1.D – Irradiance Sources 1.H – Far-side Imaging 1.F – Solar Subsurface Weather 1.E – Coronal Magnetic Field.

RHESSI and the solar radius H.S. Hudson, M.D. Fivian & H.J. Zahid Space Sciences Lab, UC Berkeley First report of our semi-intentional optical limb astrometry.

1 Pedagogical Review on Solar Cycles King-Fai Li Caltech GPS, YL Yung Group Jan 17, 2007.

Solar Radiative Output and its Variability Preethi Ganapathy November 22, 2005 Claus Frölich and Judith Lean.

Rachel Klima (on behalf of the MASCS team) JHU/APL MASCS/VIRS Data Users’ Workshop LPSC 2014, The Woodlands, TX March 17,2014 MASCS Instrument & VIRS Calibration.

June 12, 2007J. Harvey DFG-NSF Astrophysics Research Conference SOLIS A Long, Careful Look at the Sun Jack Harvey National Solar Observatory.

Solar Irradiance Variability Rodney Viereck NOAA Space Environment Center Derived Total Solar Irradiance Hoyt and Schatten, 1993 (-5 W/m 2 ) Lean et al.,

Solar Rotation Lab 3. Differential Rotation The sun lacks a fixed rotation rate Since it is composed of a gaseous plasma, the rate of rotation is fastest.

THE ROLE OF PICARD IN UNCOVERING THE PROPERTIES OF THE VARIABILITY OF THE SOLAR INTERIOR Sabatino Sofia Department of Astronomy Yale University CNES, October.

The Sun Michael J Passow. General Characteristics Our closest star Source of almost all our energy One of 100 billion in the Milky Way Galaxy “average’

Note key, please leave in binder. Our Sun

Charles Hakes Fort Lewis College1. Charles Hakes Fort Lewis College2 Doppler/ Sunspots/ Interior.

Astronomy 1020-H Stellar Astronomy Spring_2015 Day-30.

Part 4: A Special Star: Our Sun 1.  Our Dynamic Sun From NASA’s Video Gallery 2.

December in Antarctica: The Sun never sets. The images are 1 hour apart.

Energy Transport and Structure of the Solar Convection Zone James Armstrong University of Hawai’i Manoa 5/25/2004 Ph.D. Oral Examination.

Atmospheric transport and chemistry lecture I.Introduction II.Fundamental concepts in atmospheric dynamics: Brewer-Dobson circulation and waves III.Radiative.

EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens 

Notes 13 – Tools and Classification of Stars Mrs. Gordon Earth Science Friday, October 23, 2015Friday, October 23, 2015Friday, October 23, 2015Friday,

Comparison of Solar EUV Irradiance Measurements from CDS and TIMED/EGS W. T. Thompson L3 Communications EER, NASA GSFC P. Brekke ESA Space Science Department.

CE 401 Climate Change Science and Engineering solar input, mean energy budget, orbital variations, radiative forcing January 2012.

Solar Irradiance Variability and Climate

Climate Dynamics Starts with the Sun NASA Image From Wallace and Hobbs r = 6.96x10 8 m T=5780K Photosphere Sunspots Faculae Figure 1.1.

Stars Physics Astrophysics. Brightness Different brightness. Different color. How bright are they really? What is due to distance? What is due.

NoRH Observations of Prominence Eruption Masumi Shimojo Nobeyama Solar Radio Observatory NAOJ/NINS 2004/10/28 Nobeyama Symposium SeiSenRyo.

SOLAR VARIABILITY AND CLIMATE. HAS THE EARTH WARMED? Climatic Research Unit, UK.

DEVELOPING A SOLAR RADIOMETRIC CALIBRATION SYSTEM USING SPECTRAL SYNTHESIS. Peter Fox (HAO/NCAR) We present quantitative information on how we estimate.

The Sun. Heat Transport in the Sun Conduction Convection Radiative Diffusion.

National Solar Observatory Godwin, Cole. Instrumentation and Facilities Dunn Solar Telescope (Sacramento Peak) Solar adaptive optics and high-resolution.

Topics in Space Weather Earth Atmosphere & Ionosphere

Reconstruction of solar irradiance variations in cycles 21, 22 and 23 based on surface magnetic fields Thomas Wenzler Institute of Astronomy ETH Zurich.

The Sun: Part 2. Temperature at surface = 5800 K => yellow (Wien’s Law) Temperature at center = 15,000,000 K Average density = 1.4 g/cm 3 Density at center.

High resolution images obtained with Solar Optical Telescope on Hinode

Image: January 2004 Blue Marble Composite – Reto Stöckli, NASA Earth Observatory Energy, space, and Earth's effective temperature Unit 1 of Earth’s Thermostat.

Sunspot Telescope Sunspots and surface granulation are the two main features. Telescope: Celestron NexStar 5 mounted on a Losmandy mount. Field of View.

What the Long-Term Sunspot Record Tells Us About Space Climate David H. Hathaway NASA/MSFC National Space Science and Technology Center Huntsville, AL,

SCM x330 Ocean Discovery through Technology Area F GE.

Remote sensing: the collection of information about an object without being in direct physical contact with the object. the collection of information about.

Solar variability and its impact on climate Laura Balmaceda 4 th El Leoncito Solar Physics School November, 2008.

Helioseismology for HMI Science objectives and tasks* Data analysis plan* Helioseismology working groups and meetings *HMI Concept Study Report, Appendix.

To what extent does solar variability contribute to climate change? Dr. David H. Hathaway NASA/Marshall Space Flight Center National Space Science and.

한 미 려 – Introduction (1) 2.Instrument & Observe 3.Science 2.

Shivam Raval Indian Institute of Technology, India

Hauchecorne, M. Meftah, P. Keckhut,

THE SUN The star we see by day.

Hiroko Watanabe (Kyoto Univ.)

Solar Dynamics Observatory (SDO)

PSP, SO, and Ground-based Synoptic Observations from NSO

Imaging Planets FRS 120 Lecture 4.

HMI Investigation Overview

The Sun Our Nearest Star

Earth Science Ch. 24 The Sun.

TIMED SABER Data Enables Scientists to Derive a 70-year Time Series of the Thermosphere’s Infrared Energy Budget With its long, comprehensive dataset,

NASA/SOHO Satellite Images

Presentation transcript:

Irradiance Variation at Solar Minimum: Real or Instrumental? David Rust, JHU/APL Space Physics Group A Cooperative Research Project for the International Heliospheric Year (IHY) Heliospheric Year (IHY) Includes Solar Imaging, Helioseismology, Radiometers and Spectrometers at the next sunspot minimum (expected in 2007)Includes Solar Imaging, Helioseismology, Radiometers and Spectrometers at the next sunspot minimum (expected in 2007) Broad objective is to measure secular trends in solar irradianceBroad objective is to measure secular trends in solar irradiance (if any) and find their sources on the Sun. (if any) and find their sources on the Sun.

Irradiance at Solar Minimum: Project Objectives Project Objectives Does irradiance vary from one solar minimum to the next?Does irradiance vary from one solar minimum to the next? Why does the correlation with magnetic features seem to change from one cycle to the next?Why does the correlation with magnetic features seem to change from one cycle to the next? Are all variations associated with magnetic features?Are all variations associated with magnetic features? What is the irradiance when there are no magnetic features?What is the irradiance when there are no magnetic features? Are there large-scale, subtle irradiance variations associated with torsional waves, giant convection cells, meriodional flows, etc.?Are there large-scale, subtle irradiance variations associated with torsional waves, giant convection cells, meriodional flows, etc.? Do the large-scale features revealed by time-distance helioseismology cause some irradiance variations?Do the large-scale features revealed by time-distance helioseismology cause some irradiance variations? What is the baseline spectral distribution at solar minimum?What is the baseline spectral distribution at solar minimum?

Evidence that the Total Solar Irradiance at Sunspot Minimum Has Increased Using a 25-year series of satellite experiments, a minima-to-minima total solar irradiance trend of %/decade is resolved during solar cycles 21 to R. Wilson, Columbia University -- R. Wilson, Columbia University

Indices of Magnetic Activity Show No Change

Brightness of Fraunhofer Lines Shows a Secular Increase Since the Last Sunspot Minimum These results and the apparent increase in solar irradiance at sunspot minimum may be instrumental, but if they are real, the implications for climate change are profound..

Participants in the Campaign to Measure Irradiance Variations Solar Imagers: SOHO, STEREO, RISE (Radiative Inputs of the un to Earth) Network, SBI (Solar Bolometric Imager), CSUN (Cal. State University at Northridge), ground-based observatories… Solar Imagers: SOHO, STEREO, RISE (Radiative Inputs of the Sun to Earth) Network, SBI (Solar Bolometric Imager), CSUN (Cal. State University at Northridge), ground-based observatories… Helioseismological Imagers: Global Oscillations Network Group, Michelson-Doppler Imager Magnetographs: Global Oscillations Network Group, Michelson- Doppler Imager, SOLIS Solar Irradiance Monitors: ACRIM, SOHO (Virgo),TIMED, SORCE, SOLIS, NSO Calcium Line Monitor… Solar Irradiance Monitors: ACRIM, SOHO (Virgo),TIMED, SORCE, SOLIS, NSO Calcium Line Monitor…

New Instrument: Solar Bolometric Imager (SBI) SBI is a bolometric telescope = it images radiant energy of the sun. SBI is a bolometric telescope = it images radiant energy of the sun. SBI may help resolve the present controversy about the reality of long-term variations in solar irradiance. long-term variations in solar irradiance. On September 1, 2003, SBI had a successfu 9-hour flight over New Mexico aboard the JHU/APL balloon-borne gondola. Experiment science team: P. N. Bernasconi, H. A. C. Eaton, Experiment science team: P. N. Bernasconi, H. A. C. Eaton, D. M. Rust (all JHU/APL) and P. Foukal (Heliophysics) D. M. Rust (all JHU/APL) and P. Foukal (Heliophysics)

Imaging Bolometer Characteristics o 320x240 Barium Strontium Titanate (BST) ferroelectric detector elements o Pixel size: 50 x 50  m. o On-chip thermal regulation to BST Curie temperature (~30 °C). o Senses by pyroelectric and dielectric effects. o AC coupled  Frame rate 30 images per second. o Detector array covered with a thin film of gold black. o Spectral absorptance of gold black films vary less than 1%. o Absorbed radiation of different wavelengths is totally absorbed and redistributed by the gold black in form of thermal emission. o The thin uniform coating retains ~ 70% of the original detector MTF. [%]

SBI First Results 10 tiles needed to compose a full disk mosaic Each tile is the average of 60 individual frames individual frames

WN SBI bolometric image with limb darkening removed This is the first full-disk total light image of the Sun ever obtained. It is a composite of 10 separate images recorded by the SBI on September 1, Faculae, spots and enhanced network smaller than 10 arcsec are clearly resolved. Pixel-to-pixel RMS noise is about 0.2%

Irradiance Variation at Solar Minimum: Real or Instrumental? Conclusions Coordinated Solar Imaging, Helioseismology, Radiometry and Spectrometry will be required.Coordinated Solar Imaging, Helioseismology, Radiometry and Spectrometry will be required. Broad objective is to measure variations in solar irradianceBroad objective is to measure variations in solar irradiance and find their sources on the Sun. and find their sources on the Sun. New instruments will enable unprecedented precision measurements at a crucial phase of the sunspot cycle.New instruments will enable unprecedented precision measurements at a crucial phase of the sunspot cycle.