# Presentation: 656698

## Missions & Funding: A practical guide to doing  science 

- R. P. Lin
- Physics Dept & Space Sciences Laboratory
- University of California, Berkeley

- Science Idea
- Current research
- Outstanding questions
- Measurements Required
- New Instrument Development
- Mission Design
- Obtaining Community Support
- Papers & presentations
- NASA, NSF, NAS Committees
- Other factors
- Funding Opportunities
- NASA (space-based)
- NSF (ground-based)
- Foreign

## Slide 3

## 23 July 2002 X4.8 Flare(Lin et al 2003)

- Thermal Plasma
- 	~3x107 K
- Accelerated Electrons
- ~10 keV to >10s MeV
- Accelerated Ions
- ~1 to >100s of  MeV

## The Sun is the most energetic particle    accelerator in the solar system:		- Ions up to  ~ 10s of GeV  		- Electrons up to ~100s of MeV			Acceleration to these energies occurs in transient energy releases, in two (!) processes:		- Large Solar Flares, in the lower corona		- Fast Coronal Mass Ejections (CMEs), in 		the inner heliosphere, ~2-40  solar radii	

## 
  Large (L)SEP events 

 	- tens/year at solar maximum 

	- dominated by: 	- >10 MeV protons (small e/p ratio)
	         		- Normal coronal composition (?)
				- Normal coronal charge states (?)

	- SEPs seen over  >~100o of solar longitude

	- associated with: - Fast Coronal Mass Ejections (CMEs)
				- Large flares (but sometimes missing) 
				- Gradual (~hours) soft X-ray bursts 
				      (also called  Gradual SEP events)		
* Acceleration by fast CME driven shock wave  	in inner heliosphere, ~2-40 solar radii

-   _Large (L)SEP events__ _
* **	**- tens/year at solar maximum*
- 	-* dominated by: **	**- >10 MeV ****protons ****(small e/p ratio)*
*	**         **	**	**- Normal coronal composition (?)*
*	**	**	**	**- Normal coronal charge states (?)*
*	**- SEPs seen over  >~100**o of solar longitude*
*	**- associated with: - Fast Coronal Mass Ejections (CMEs)*
*	**	**	**	**- Large flares (but sometimes missing) *
*	**	**	**	**- Gradual (~hours) soft X-ray bursts *
*	**	**	**	**      **(also called  *_Gradual SEP events__*)*_*	**	*
- * Acceleration by fast CME driven shock wave  	in inner heliosphere, ~2-40 solar radii
*	**	**	*
*	**	**	** **	**	**	*

## Slide 8

## Slide 10

## Slide 11

- Science Idea
- Current research
- Outstanding questions
- Measurements Required
- New Instrument Development
- Mission Design
- Obtaining Community Support
- Papers & presentations
- NASA, NSF, NAS Committees
- Other factors
- Funding Opportunities
- NASA (space-based)
- NSF (ground-based)
- Foreign

## <----- RHESSI coverage ----->

- Π0 Decay

- Nonthermal Bremsstrahlung

- Thermal Bremsstrahlung

- Solar Flare Spectrum

- Positron and Nuclear
- Gamma-Ray lines

- T = 2 x 107 K

- T = 4 x 107 K

- hot loop

**    ****HXR**
**footpoints**

**soft X-rays                hard X-rays**

******-rays ******

- photosphere

## Slide 14

## Grid #3

## Angular Coverage Vs. Energy

## 	Detector Design

- 	**Detector Design**

## Germanium Detector Housing

**Germanium Detector Housing**

## Energy Resolution vs. Energy

## Instrument Development

- HIREGS (High Resolution Gamma-ray/Hard X-ray Spectrometer)
- Long Duration Balloon Payload flown in Antarctica 1991-2
- HEIDI (High Energy Imaging Device)
- Demonstration Balloon flight 1993

## Slide 21

## Slide 22

- Science Idea
- Current research
- Outstanding questions
- Measurements Required
- New Instrument Development
- Mission Design
- Obtaining Community Support
- Papers & presentations
- NASA, NSF, NAS Committees
- Other factors
- Funding Opportunities
- NASA (space-based)
- NSF (ground-based)
- Foreign

## Community Support

- NASA
- Heliophysics (Sun-Earth Connections)Roadmap
- National Academy of Science
- Committee on Solar & Space Physics (CSSP)
- Solar & Space Physics Decadal Survey
- Studies
- NASA –Science & Technology Definition Team
- NSF – similar for ground-based oservatories

## Other Factors

- NASA’s Vision for Space Exploration
- Humans to Moon & Mars

## Funding opportunities

- Solar Terrestrial Probes ~$500M
- STEREO, MMS, GEC
- Living with a Star (LWS) ~$500M
- SDO, Geospace (RBSP, ITSP), Sentinels
- Explorers
- Small Explorers (SMEX) ~$100M
- Middle Class Explorers (MIDEX) ~$250M
- Supporting Research & Technology (SRT)
- Low Cost Access to Space (LCAS): Rockets & Balloons
- Flagship Missions
- Solar Probe ~$1B

## Proposals 

- Forming a team
- Scientific, technical, financial, managerial
- Maximize science
- Minimize risk
- 	Instrument Design
- 	Mission Design
- 	Spacecraft
- 	Mission Operations & Data Analysis

## Development (Fabrication)

- Instrument(s)
- Spacecraft
- Usually subcontractor
- Integration & Test
- Ground system
- Data downlink
- Mission Operations Center (MOC)
- Science Operations Center (SOC)

## Reviews

- Competition
- Science  ~40% - Peer review
- Implementation  ~30%
- Management & cost ~30%
- TEMCO (Technical, Management, Cost) Review

## Germanium Detector Housing

**Germanium Detector Housing**

## Mechanical Cryocooler

## Slide 33

## Front Tray

## Rear Tray

## Imager – side view

## CCD RAS

## DavePankow

**Dave****Pankow**

**Paul****Turin**

## RHESSI vibration test anomaly

**Notes:**
13.

##   SPACEFLIGHT NOW
	Posted: June 4, 2001
   X-43A launch failure

   Next Pegasus rocket launch delayed in X-43A aftermath   
  	The High Energy Solar Spectroscopic Imager, or HESSI satellite, was scheduled to rocket into space on Thursday aboard an air-launched Orbital Sciences Pegasus XL booster. 

- 	Posted: June 4, 2001
**   ****X-43A launch failure**
-    **Next Pegasus rocket launch delayed in X-43A aftermath**
-   	The High Energy Solar Spectroscopic Imager, or HESSI satellite, was scheduled to rocket into space on Thursday aboard an air-launched Orbital Sciences Pegasus XL booster.

## Slide 42

##  RHESSI launch February 5, 2002

-  RHESSI launch February 5, 2002

## Slide 44

## U.C. Berkeley Mission Operations Center

- BGS Antenna, Equipment Racks and FOT Workstations at the UCB Mission Operations Center

## Slide 46

**Notes:**
showresolution

## Reuven Ramaty (1972)1937 – 2001 

## Imaging spectroscopy

## Slide 49

## Spectral Components

- 511 keV- positron annihilation

- Neutron-capture2.2 MeV

- power law - electron bremsstrahlung

- De-excitation lines -narrow

- broad

- total model

## Electrons vs protons

- 200-300 keV HXR (electrons) footpoints are moving along ribbons
- 2.2 MeV image (protons)
- is averaged over 22 min, delayed by ~100 s from electrons
- CONCLUSIONS:
- Electrons and protons both close to ribbon, but separated by ~104 km

- Data Analysis
- Workshops & Meetings
- Extended Mission
- Senior Review

## The Living With a Star (LWS) Sentinels Mission

- R. P. Lin
- University of California, Berkeley
- Szabo, Study Scientist
- NASA Goddard Space Flight Center
- & the Sentinels STDT
- (Science & Technology Definition Team)

## Sentinels STDT

**Stuart D. Bale****	****	****UCB****	****	****Joseph M Davila****	****	****GSFC**
**Antoinette B. Galvin****	****UNH****	****	****Dennis K. Haggerty****	****APL**
**Stephen W. Kahler****	****AFRL****	****	****Joseph E. Mazur****	****              Aerospace**
**Richard A. Mewaldt****	****Caltech****	****	****Neil Murphy****	****	****JPL**
**Geoff D. Reeves****	****	****LANL****	****	****Pete Riley****	****	****SAIC**
**James M. Ryan****	****	****UNH ****	****	****Karel Schrijver****	****	****Lockheed**
**Rainer Schwenn           MPI Lindau****	****Allan J. Tylka****	****	****NRL**
**Thomas Zurbuchen****	****U Mich**
**	****	****Robert F. Wimmer-Schweingruber****	****University of Kiel**
**	****	****	****Ex-Officio and other non-members:**
**Adam Szabo****	****	****GSFC ****	**** ****	****Sentinels Study Scientist **
**Michael Wargo****	****	****NASA/HQ****	****Exploration Representative**
**Lika Guhathakurta  ****	****NASA/HQ   ****	****Program Scientist****	****	**
**Chris StCyr****	****	****GSFC****	****	****LWS Sr. Project Scientist**
**Haydee M. Maldonado****	****GSFC****	****	****Project Manager**
**Hermann Opgenoorth****	****ESA****	****	****ILWS Chair****	****	****       **
**Ronald D Zwickl****	****	****NOAA/SEC****	****User Community Representative****	****	****	**

**Sentinels STDT**

## Sentinels Primary Objective

**Sentinels Primary Objective**

## Sentinels Science Questions

- What is the origin/source of the see particles?

- How, when and where areenergetic particles accelerated?

- What is the role of CMEs and flares producing SEPs?

- How are the highest energy solarparticles (>100 MeV/nuc) produced?

- How do SEPs propagate in the inner heliosphere?

- What determines the radial, longitudinaland latitudinal distribution of SEPs?

- How are CMEs initiated? Constraints on models andmechanisms.

- What is the internal structure and solar connection ofICMEs? (Why do many CMEs become irregular ejecta?)

- How do ICMEs propagate and evolve?

- What is the structure, propagation and evolution ofinterplanetary shocks?

- How do the heliospheric magnetic fields and plasmaconnect to and disconnect from the solar corona?

- How do the fast and slow streams interact to formthe heliosphere?

- What is the origin of waves and turbulence and theirsignificance for particle acceleration and dissipation?

- SEP Source Population

- SEP Acceleration

- SEP Propagation

- ICMEs

- IP Shocks

**SEPs**

**Transients**

**Global Structure of the****Inner Heliosphere**

## Sentinels in Exploration

-  Determine where, when and how are solar energetic   particles (SEPs) accelerated.
-  Determine how energetic particles propagate and   and are modulated.
-  Characterize the interplanetary   environment   (worse case scenarios)
-  Develop forecasting capabilities   for Earth, Mars  and for   spacecraft in transit.

## Inner Heliosphere Sentinels (IHS) Mission

**Launch Vehicle:**
**Atlas 5 ELV, 4 S/C Single Launch**
**Launch Date: 4 Sept 2015**

**Inner S/C Final Orbit 0.250 x 0.740 AU**
**First Min Perihelion Pass ******** 2.49 Yrs from launch**

**Outer S/C Final Orbit 0.257 x 0.744 AU**
**First Min Perihelion Pass ******** 3.12 Yrs from launch**

**Science & Tlm Dwnlnk to DSN , One 8 hr Pass/wk; S/C Cmnds thru DSN**

**Continuous Space Weather Non-DSN Link**

**Spacecraft Concept:**
**Mass:****	****~580 kg. wet**
**Power:****	****~300-660 W**
**Data Rate:****	****~7 kbps**
**Life:****	****3 yr design, 5 yr goal**

## Deployed Configuration

- Dual Magnetometer

- Wire Antenna

- Wire Antenna

- SW Electrons/
- Search Coil

- HEI-C

- Radio Stacer

## Ballistic trajectory that minimizes time to 60 degrees and then drifts from 60 to 180 degrees in < 4 years
C3 = 3.901 km2/s2
Delta-V = 1.150 km/s (includes 144 m/s)
Launch Vehicle:  Delta II 2925H (delivers 921 kg dry mass)

- C3 = 3.901 km2/s2
- Delta-V = 1.150 km/s (includes 144 m/s)
- Launch Vehicle:  Delta II 2925H (delivers 921 kg dry mass)

- Imaging Sentinel

## ESA Solar Orbiter and Sentinels

-  Inner heliospheric (0.22 x 0.9 AU) mission  in the same time frame as IHS.
-  Both in-situ and remote sensing instrumentation.
-  2nd half of mission to latitudes above 30°.

## The Phases of Sentinels

**WIND, ACE**

**STEREO**

**SDO**

**Inner Heliospheric****Sentinels**

**ESA****Solar Orbiter**

**Imaging Sentinel**

**Phase 1**

**Phase 2**

**Solar Cycle**

**The Phases of Sentinels**

- Inner Heliospheric
- Sentinels

**Solar Orbiter**

- Sentinels

## LWS Sentinels will develop the physical understanding necessary to reliably model and predict the radiation environment for Lunar and Martian missions. Sentinels will accomplish this by discovering the physical conditions and mechanisms that govern SEP production and transport in the heliosphere. 

LWS Sentinels will develop the technical understanding necessary to implement a future heliospheric space weather warning system.  Sentinels will have real-time capabilities that allow testing of space weather monitoring/forecasting functions.

- LWS Sentinels will develop the technical understanding necessary to implement a future heliospheric space weather warning system.  Sentinels will have real-time capabilities that allow testing of space weather monitoring/forecasting functions.

-          Relation to Exploration

## Timing of Sentinels

**2000**

**2010**

**2020**

**2030**

**Return to the Moon**
**2015-2020**

**On to Mars**
**Date TBD**

**SDO**

**STEREO**

**SOHO**

**ACE**

**Sentinels**

- Only One More Solar Cycle Left to Learn What We Must Learn

**Cycle 24**

## Slide 65

## Slide 66

## Mewaldt et al 2004

## If these SEPs are accelerated by CME-driven shocks, they use a significant fraction of the shock kinetic energy (~3% to 20%)

**(see also Emslie et   al. 2004). **

## In the Jan 20 Event the high energy particle-intensities reach Earth just minutes after the x-rays from the flare (Mewaldt et al 2005)

## Timing

- Red vertical line (06:48UT):
- Solar release time assuming first arriving particles travel at v=c along L=1.2 AU
- HXRs peak at 06:45:00UT
- 2.2 MeV peak at 0647:30UT
- 06:54UT: CME at ~3 Rsun
- Line: 2500 km/s CME speed
- Red crosses: Rising SXR loops

## Krucker et al 2005

## Proton spectrum:RHESSI  Gamma-rays (lines) vs SEPs at 1AU(blue points)

- Proton spectrum:RHESSI  Gamma-rays (lines) vs SEPs at 1AU(blue points)

## Inner Heliospheric Orbit Design

**IHS 3**

**IHS 1**

**IHS 4**

**IHS 2**

- 44°

-  3 Venus gravity  assists for each  spacecraft
-  Final orbits:  0.25 x 0.76 AU
-  Orbital periods:  127-136 days
-  Cruise:  2 yr 3-11 months to final configuration, Science starts 60 days after launch
-  Launch opportunities:  (2012 May) 2014 Feb,   2015 Sept

**Venus**

**Mercury**

**Earth**

## Slide 74