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A1309.01. Imaging Parameters A1309.01 Imaging Parameters A1309.01.

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Presentation on theme: "A1309.01. Imaging Parameters A1309.01 Imaging Parameters A1309.01."— Presentation transcript:

1 A1309.01

2 Imaging Parameters A1309.01

3 Imaging Parameters A1309.01

4 HESSI A1309.02

5 HESSI Science Objective  Impulsive Energy Release in the Corona  Acceleration of Electrons, Protons, and Ions  Plasma Heating to Tens of Millions of degrees  Energy and Particle Transport and Dissipation To explore the basic physics of particle acceleration and explosive energy release in Solar Flares A1309.03

6 HESSI Non-Solar Science Objectives  The Crab Nebula – Imaging spectroscopy with 2” resolution  Gamma Ray Bursts and Cosmic Transient Sources – Detected over a large fraction of the sky – High resolution spectroscopy – Search for cyclotron line features  Steady X-ray and gamma-ray sources (point and diffuse) – Detect by Earth occultation or through the rear grids – Obtain high resolution spectra – Search for line features A1309.04

7 HESSI Primary Observations  Hard X-ray Images – Angular resolution as fine as 2 arcseconds – Temporal resolution as fine as 10 ms – Energy resolution of <1 keV from 3 keV to 400 keV  High Resolution X-ray and Gamma-ray Spectra – keV energy resolution –To energies as high as 20 MeV A1309.05

8 Complementary Observations SOHOEUV images and spectra Coronagraph images Particle spectra and abundances GOESImages from the Soft X-ray Imager ACEEnergetic particle spectra and abundances Ground-based Observatories Radio and optical images and spectra Magnetograms A1309.06

9 HESSI Firsts  Hard X-Ray Imaging Spectroscopy  High Resolution Spectroscopy of Solar Gamma-Ray Lines  Hard X-Ray and Gamma-Ray Imaging above 100 keV  Imaging of Narrow Gamma-Ray Lines  High Resolution X-ray and Gamma-Ray Spectra of Cosmic Sources  Hard X-Ray Images of the Crab Nebula with 2- arcsecond Resolution A1309.07

10 Relevance to Strategic Plan  Part of the Solar Connections Program - in the Roadmap for the next solar maximum.  Seeks to understand fundamental physics of solar flare energy release and particle acceleration.  Relevant to understanding relation between flares and coronal mass ejections and their effects on the Earth and its environs. A1309.08

11 Expected Numbers of Flares MicroflaresTens of thousands Hard X-ray flares with crude imaging and spectra>1000 to >100 keV Hard X-ray flares with >10 3 counts s -1 detector -1 Hundreds above 20 keV allowing spatial scales to be followed on timescales of 0. I s Flares sufficiently intense to allow the finestTens possible imaging spectroscopy Flares with the detection of gamma-ray linesUp to 100 Flares with detailed gamma-ray line spectroscopyTens and the location and extent of the source determined to ~40 arcseconds A1309.09

12 HESSI Observational Characteristics  Energy Range3 keV to 20 MeV  Energy Resolution~1 keV from 3 keV to 1 MeV Increasing to 5 keV at 20 MeV  Angular Resolution2 arcseconds to 40 keV 7 arcseconds to 400 keV 36 arcseconds to 20 MeV  Temporal ResolutionTens of ms for basic image 2 s for detailed image  Field of ViewFull Sun  Effective Area - cm 2 10 -3 at 3 keV, 1 at 10 keV 100 at 100 keV, 50 at 10 MeV  Numbers of flares~1000 imaged to >100 keV. ~100 with spectroscopy to ~10 MeV A1309.010

13 HESSI Summary Instrument9 germanium detectors (7-cm dia. x 8 cm) Cooled to 75 K with Sunpower cooler Grid pitches from 34 microns to 2.75 mm 1.5-m grid separation Solar Aspect System to <1 arcsecond Roll Angle System to 1 arcminute Weight120 kg Power110 watts Telemetry<11 Gbits/day SpacecraftSpinning at 12 - 20 rpm Pointing to within 0. 1° of Sun center Launch VehicleSELV(TBD) Orbit38° inclination 600 km altitude, >3-year life Launch Datemid-2000 Operations3 years A1309.011

14 HESSI PI and Co-Is Robert LinUniversity of California, BerkeleyPI Brian DennisGSFC/682Mission Scientist Carol CrannellGSFC/682Education & Outreach Gordon HolmanGSFC/682Flare Theory Reuven RamatyGSFC/661Flare Theory Tycho von RosenvingeGSFC/661ACE Collaboration Patricia BornmannNOAAGOES Collaboration Richard CanfieldMontana State UniversityGround-based Observations Gordon EmslieHuntsvilleFlare Theory Hugh HudsonSolar Physics Research Corp.Imaging Gordon HurfordCaltechImaging Norman MaddenLBNLGermanium Detectors Arnold BenzInst. of Astronomy, Zurich, SwitzerlandRadio Observations John BrownUniv. of Glasgow, ScotlandFlare Theory Shinzo EnomeNAO, JapanRadio Observations Takeo KosugiNAO, JapanImaging Frank van BeekDelft Univ., The NetherlandsGrids and Imaging Nicole VilmerObservatoire de Paris, Meudon, FranceData Analysis Alex ZehnderPaul Scherrer Inst. SwitzerlandTelescope design and fabrication A1309.012

15 HESSI Prime Responsibilities UC BerkeleyGermanium detectors & electronics I & T Ground station, MOC/SOC Data Analysis GSFCGrid characterization & testing Cooler, cryostat design Data analysis, distribution, and archiving PSI (Switzerland)Telescope & aspect system JPLFinest grids (#1 & 2) van Beek (The Netherlands)Coarser grids (#3 - 9) & mounts Spectrum AstroSpacecraft A1309.013

16 GSFC Involvement Science Dennis (682)Mission Scientist Hurford (Caltech)Imaging Scientist Holman (682), Ramaty (661)Solar flare physics Aschwanden (UMd)X-ray interpretation von Rosenvinge (661)ACE/HESSI coordination Crannell (682)Education & Public Outreach Imaging Clark (750), Amato (686)Grid environmental testing Orwig (682), Lang (CUA), Uribe (HSTX)Optical & X-ray grid characterization Schmahl (UMd)Image reconstruction Spectrometer Boyle (713)Cryostat design, cooler evaluation Provide flight-qualified Sunpower cooler Schwartz (HSTX)Spectral deconvolution Data Analysis Gurman (682), Zarro (ARC)Solar Data Analysis Center Tolbert (HSTX)Data archiving and distribution A1309.014

17 Test Fine Grids A1309.015

18 Germanium Detector A1309.019

19 Sunpower M77 Stirling-Cycle Cooler A1309.020

20 Instrument Sensitivity A1309.021

21 Angular Coverage vs. Photon Energy A1309.022

22 Relative Modulation Amplitude vs. Photon Energy A1309.023

23 Energy Resolution vs. Photon Energy A1309.024

24 Count Rates in Each Detector for One Rotation A1309.025

25 Prelaunch Twist Monitoring System (TMS) A1309.026

26 A1309.027

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