# Presentation: 532491

## Future instrumentation for high-energy

-     solar physics
-               a partial and partial survey
-                             David Smith

## Future instrumentation for high-energy

-     solar physics
-               a partial and partial survey
-                             David Smith

- Crystal ball

## Future instrumentation for high-energy

-     solar physics
-               a partial and partial survey
-                             David Smith

- Crystal ball

- OK, it's really the neutron and gamma-ray
- detector proposed for Solar Orbiter

## Future instrumentation for high-energy

-     solar physics
-               a partial and partial survey
-                             David Smith

- Crystal ball

- OK, it's really the neutron and gamma-ray
- detector proposed for Solar Orbiter
- But it **IS **a crystal ball, anyway

## Part 1: upcoming missions

-                 Near term
-                 Further out
- Part 2: evolving technologies

## STEREO: launch in 1 month!

- http://stereo.gsfc.nasa.gov/instruments/instruments.shtml
-            LET/HET: dE/dx vs E technique for high-energy particles
-            suprathermal electron telescope 2-20 keV, Si
-            radio waves instrumentation
-            also: EUV, white light, plasma composition

- Suprathermal electron telescope
- Graphic: U. C. Berkeley

- Graphics: NASA

## Solar-B (Japan/US/UK)  Launch this year!

-      (Solar-A was Yohkoh)

- http://www.isas.ac.jp/e/enterp/missions/solar-b/

- Optical telescope:
-      Filter vector magnetograph
-      Spectropolarimeter
-      Subarcsec resolution, active region FOV
- Soft x-ray telescope:
-       2" resolution, full sun FOV
- EUV  imaging spectrometer:
-       Few arcmin FOV
-       2" resolution
-       Dispersive slit spectroscopy
-       Wavelength ranges: 170-210A, 250-290A

- G

- Graphics: JAXA

##        CORONAS-Photon; Launch 2007, third in a series of Russian

-        CORONAS-Photon; Launch 2007, third in a series of Russian
-                 solar spacecraft, part of ILWS.  LEO.
-        Strategy is many smaller, somewhat redundant instruments
-        Led by Moscow Engineering Physics Institute (State University)
-                 http://www.astro.mephi.ru/english/e_photon/e_instr.htm
-         5 high-energy photon instruments (including Penguin polarimeter)
-         2 high-energy particle instruments
-         UV, magnetometer, etc.

- Graphic: MEPhI

## G

- GLAST:  Launch 2007, NASA/DOE astrophysics mission

-  LAT  (Si tracker)  > 30 MeV (Pion range)
-  Burst Monitor -- NaI/BGO -- line range
-       (comparable to instruments on CORONAS)
-  http://glast.gsfc.nasa.gov/

- Graphics: NASA

## Solar Dynamics Observatory (Launch Aug. 2008)

- No direct high-energy measurements, but superb
-    Magnetograms
-    Optical images
-    EUV irradiance measure
-           http://sdo.gsfc.nasa.gov/

- Graphic: NASA

## Missions -- further out

## FASR: Expected completion in 2010

**FASR: **Expected completion in 2010

- Combines broad spectral coverage,
- high time resolution, high spatial
- resolution -- an enormous data rate!

- Simulation of
- expected image
- quality

- Imagine an image of this quality for
- each spectral and temporal bin of
- a spectrogram:

**AUI,**
**NRAO/NSF,**
**NJIT, et al.**

- http://www.ovsa.njit.edu/fasr/

**G**

- Graphics: NJIT/NSF

## Inner heliosphere sentinels (LWS):

- Inner heliosphere sentinels (LWS):

-         Full high-energy particle suite
-         Gamma-ray spectrometer (LaCl3, LaBr3, or NaI)
-         Neutron spectrometer/imager
-         Hard x-ray imager (may spin either way, CZT & Si detectors)
-               Close-in stereoscopy, far side as well
-         Plasma, magnetometer, waves instruments

- Graphic: NASA

## Solar Orbiter 

-         http://sci.esa.int/science-e/www/area/index.cfm?fareaid=45
-         Launch ~2015; approach as close as 45 solar radii (0.2 AU)
-         Payload definition document includes
-             "Neutron Gamma-ray Detector" (NGD):
-                  5kg,  0.6-20 MeV (n), 0.05-10 MeV(g)
-                  LaBr3 inside, boron-doped plastic anticoincidence & n-detector
-             "Energetic Particle Detector" (EPD), 2 keV - 100 MeV, 8.1 kg
-             "Spectrometer telescope imaging x-ray" (STIX), bigrid, CZT,
-                   nonrotating (Yohkoh style), 3-150 keV, 4 kg

- Graphics: ESA

## Far-off astrophysics missions with good flare science:

- Black Hole Finder Probe (CASTER or EXIST):
-     Huge all-sky monitor; detectors sensitive from 5 or 10 keV
-     up to 200 or 600 keV, coded masks, very large area.
-     Good nanoflare sensitivity.  Unlikely before 2020.
- Advanced Compton Telescope (ACT):
-     High sensitivity, possibly high resolution, 300 keV to 30 MeV range;
-     Unlikely before 2020.

## Will we get a flare MIDEX by 2020?

**Will we get a flare MIDEX by 2020?**

## Slide 17

## Part 2: Emerging technologies

## Some recent detector advances:

**Some recent detector advances:**

- Lanthanum scintillators (LaCl3, LaBr3):
- Resolution 2-3 times better than NaI,
- more stopping power, 10x faster response.
- 3"x3" available as of June 1! (so says
- the manufacturer, Saint-Gobain)

- Germanium strip detectors:
- Full Ge resolution
- Full 3-d position of every interaction to 1mm
- Enables Compton tracking for:
-         Crude imaging
-         Background rejection
-         Rejection of incomplete collection
-         Polarimetry

- Graphics:
- St-Gobain Inc.

- Graphic: S. Boggs, UCB

## Some recent advances in imaging:

- Laue-lens focusing for MeV
- gamma-rays in a narrow energy
- band.  Being designed for
- astrophysics at nuclear line bands,
- but some of these (511, 847) are
- good for solar, too.  Optimize for 2.2 MeV?
- CLAIRE balloon, P. von Ballmoos, CESR Toulouse

- Multilayer-coated grazing incidence
- optics; high/low Z thin layers (e.g.
- W/Si).  Interference-based, too, but
- longer wavelengths.  Extend
- capabilities of mirrors from ~10 keV
- to ~70 keV.  Good possible use for
- nanoflare studies.
- SIMBOL-X, ESA; [NuSTAR, NASA]

- Graphics:
- P. von Ballmoos

- Graphic:
- Caltech/LLNL

## Advanced neutron detection (here at UNH):  SONTRAC

- Energy range: 20-250 MeV neutrons (and gammas, protons,                                   electrons....)
- Scintillating plastic fibers, layered in crossed directions
- Images recoil protons, gets direction as well as energy, 3D!
- Greatest potential is near
- the Sun, where neutrons
- at lower energies are
- still undecayed.

- Graphic: J. Ryan,
-               UNH

## Microcalorimeters for nondispersive, high resolution thermal 

**                                       ****x-ray spectroscopy**

- XRS microcalorimeter for Suzaku
- (Graphic: NASA Goddard)

- Combines high energy resolution like
- a bent-crystal or other dispersive
- spectrometer with wider energy range
- and true 2D imaging of a Si or
- CZT pixel detector.
- Requires 60 mK operation.
- Resolution around 10 eV
- from 0.2 to 10 keV
- Unit on Suzaku (AstroE2), an
- astrophysics mission, had a failure
- in its cooling system soon after launch

## Wanted: a way to detect ions at the Sun below the 2 MeV threshold

**for the beginning of nuclear lines**
- Protons in flight can charge-exchange with thermal neutrals when
-     they reach 40 keV; results in atomic lines with strong redshifts.
- Gives an integral measure of total proton flux above 40 keV.
- Lyman-alpha red wing can be dominated by this effect.
- Requires neutral H -- look at start of flare.
- UV telescope must strongly suppress line center.
- Similar technique used to image proton aurora on Earth (IMAGE
-       satellite, instrument led by S. Mende).

## [YOUR IDEA HERE]