# Presentation: 592308

## Russian magnetospheric & 

**heliospheric missions**

## CORONAS-PHOTON  

**CORONAS-PHOTON  **
**Solar imaging and spectroscopy from EUV to 2000 MeV**
**To be launched in fall 2008**

**Moscow Engineering**
**Physics Institute**
**Yu. Kotov**
**http://iaf.mephi.ru**

**Currently flight payload is **
**delivered. **
**Completion of satellite **
**Preparation is expected in August  **

## Solar-terrestrial payload onboard SPECTR-R

**Solar-terrestrial payload onboard SPECTR-R**

**  ****space VLBI project. **
**  ****10-meter radio telescope **
**  ****orbit with apogee   350 000 km**
**  ****launch in late 2008 or 2009**
**  ****Currently main flight payload is ****	****under integration test**
**PLASMA-F **is solar-terrestiral payload of opportunity onboard SPECTR-R.
- will be delivered after competion of main payload tests.
**Targets: **
-     Fine-scale solar wind, IMF, SCL
- 	up to 32 samples/sec
-    Solar wind, IMF, SCL monitoring

**Project Scientist:**  G.N.Zastenker   		gzastenk@iki.rssi.ru

##       PLASMA-F instruments

**Magnetic field instrument MMFF – Russia **
- 	2 DC magnetometers
- 	2 AC magnetic sensors (10 Hz – 100 kHz)
- 			PI:   A. Skalsky,   IKI, w/part LSC
**Fast solar wind monitor BMSW   - Czech R., China   **
- 	6 Faraday cups with possibility of instantaneous
- 	solar wind velocity vector and density determination
- 			PI:   G. Zastenker, IKI, w/part ChU, CSS
**Energetic particle instrument  MEP2 – Slovakia, Greece**
- 	geometric factor ~ 1
- 	electrons 15-350 keV
- 	ions 15- 3200 keV
- 			PI:   K. Kudela, IEP, w/part DUTH/SSL, IKI
**Data management system SSNI-2 – Russia **
**	**100 GB onboard memory
- 	possibility of intelligent data handling and compression
- 			PI:  L. Chesalin, IKI

## RESONANCE

-            *Space Research Institute, Moscow*
* **          **Institute of Applied Physics**,** N**.**Novgorod*
*European participation*

**RESONANCE**

**Magnetosynhronous orbit**
- Apogee: ~30 000 km,
- Perigee: ~ 1 800 km,
- Inclination: + and - 63.4o (two S/C)
- Co-rotation magnetic tube:        up to 3 hours
- Launch: 2012 on schedule
- Currently change from 2x300 kg to 4x150 kg
- satellites is considered.

**http://resonance.romance.iki.rssi.ru**

## ~ 1-10 km

**~ 1****-10**** km**

**~****1****000****-**** ****5****000**

**~**** ****5000-15000**

## RESONANCE

**RESONANCE**

**Space weather-related**
-    Ring current and outer radiation belt dynamics
-    Plasmasphere & plasmapause dynamics

**M****agnetospheric cyclotron maser**                   **Auroral region processes**
-   Interaction of electrons and waves                  small scale acceleration zones

## RESONANCE

**Launch 2012:  will operate with**
**   ****Radiation Belt Storm Probes by NASA LWS **
**   ****ERG **
**   ****ORBITALS  **
**                      ****ILWS inner magnetosphere constellation in 2012 ?**

## Small satellite platform KARAT for scientific projects

**Small satellite platform KARAT for scientific projects**
**Dry weight ~ 100 kg plus up to 60 kg of payload**
**First launch in 2009**
**Later used in Resonance, etc**

## Mini-spacecraft for magnetospheric science

**Mini-spacecraft for magnetospheric science**

- Possible collaboration with future MMS / X-scale projects

- Sci payload weight   ~ 40 kg

## Interhelioprobe

**MAIN SCIENTIFIC GOALS**** **
**mechanisms of the coronal heating and solar wind**
**fine structure and dynamics of the solar atmosphere**
**origin and the global dynamics of solar flares and CMEs**
**generation and propagation of solar energetic particles**
**mechanism of the solar dynamo and solar cycle **
**high latitudes studies**

**Interhelioprobe**

**Launch 2014.   **
**In fall 2008 decision to start phase B will be taken.**

**Notes:**
Здесь перечислены основные научные цели проекта. Они состоят в том, чтобы
Here the basic scientific goals of the project are listed. They are, that
to identify mechanisms of the coronal heating and solar wind;
to investigate the fine structure and dynamics of the solar atmosphere 
to determine the origin and study the global dynamics of the most powerful solar activity phenomena (solar flares and CMEs) and their influence on the heliosphere and space weather;
to investigate generation and propagation of solar energetic particles;
to observe from high latitudes and to investigate the solar atmosphere and corona in the polar and equatorial regions;
to determine the mechanism of the solar dynamo and solar cycle.

## INTERHELIOPROBE

**Start from the Earth**

**INTERHELIOPROBE**

**Multiple**
**Venus **
**Flight-by**

**Inclination of the orbit**

**Notes:**
Здесь показана траектория перелета КА во внутренню гелиосферу, на близкие расстояния к Солнцу - до 30 солнечных радиусов. КА стартует c Земли и за счет многократных гравитационных маневров у Венеры приближается к Солнцу, экономя за счет этого топливо и сокращая время перелета на рабочую орбиту. Гравманевры у Венеры позволяют также наклонить плоскость орбиты КА к плоскости эклиптики.

This is a trajectory of spacecraft flight in inner heliosphere, on close distances to the Sun - up to 30 solar radiuses. Spacecraft will start from the Earth and due to multiple gravitational maneuvers at Venus comes nearer to the Sun, saving due to it fuel and reducing time of flight for an operational orbit. Gravitational maneuvers at Venus also allow to incline a plane of spacecraft to ecliptic plane.

До настоящее времени все наблюдения Солнца (не  имея ввиду локальные измерения, например Ulysses) выполнялись исключительно с Земли или с околоземной орбиты. Гелиоцентрическая орбита Интергелиозонда, когда КА будет занимать разные положения по отношению к линии Солнце-Земля, имеет ряд преимуществ, которые позволяют выполнить новые виды наблюдений.

Up to the present of time all observations of the Sun (not having in view of local measurement, for example Ulysses) were carried out exclusively from the Earth or from a near-Earth orbit. Heliocentric orbit of Interhelioprobe when the spacecraft will be in different positions with respect to the line Sun-Earth, has a number of advantages which allow to carry out a new kinds of observations.

## INTERHELIOPROBEHigh resolution observations

- Fine structure and dynamics of solar atmosphere:
- magnetic network;
- magnetic flux elements; turbulence.

- Supergranulation and its role in large-scale dynamics of magnetic field and corona

- Small-scale magnetic activity:
- loops dynamics and motions of its footpoints, microflares, reconnection.

**Notes:**
Приближение КА к Солнцу позволит при том же угловом разрешении телескопа наблюдать меньшие масштабы на Солнце.  Это необходимо, например, для изучения тонкой структуры и динамики солнечной атмосферы – магнитной сетки, магнитных элементов, турбулентности, а также для наблюдений супергрануляции и магнитных петель, таких явлений как микровспышки и пересоединение.

Approach of spacecraft to the Sun will allow observe at the same angular resolution of telescope smaller scales on the Sun. It is necessary, for example, for studying fine structure and dynamics of solar atmosphere - a magnetic network, magnetic elements, turbulence, and also for observations of supergranulation and magnetic loops, such phenomena as micro flares and reconnection.

## INTERHELIOPROBEIn - situ  measurements  near  the Sun

- Distribution function. Remnants of coronal heating and related plasma  processes.

- Wave-particle interactions.

- Beams. Temperature anisotropy.
- Radio emission. Neutrons.

**Notes:**
Локальные измерения вблизи Солнца пока не проводились. Такие измерения важны для решения целого ряда проблем в физике Солнца. Это нагрев солнечной короны и ускорение солнечного ветра, природа турбулентности и ускорения частиц и др. Можно будет измерить

Local measurements near the Sun were not carry out yet. Such measurements are important to solve a lot of problems in solar physics. It is coronal heating, solar wind acceleration, a nature of turbulence and particles acceleration, etc. It will be possible to measure
Distribution function. Remnants of coronal heating and related plasma processes.
Wave-particle interactions. Waves and particles diagnostics.
Beams. Temperature anisotropy. Waves and turbulence generation. Radio emission. Neutrons.

## INTERHELIOPROBE

**     ****Optical telescope**
**     ****Magnetograph     **
**     ****X-ray imager-spectrometer**
**     ****Coronograph**
**     ****HELIOSPHERIC INSTRUMENTATION**
**     ****Solar Wind Ion Analyzer **
**     ****Solar Wind Electron Analyzer **
**     ****Solar Wind Plasma and Dust Analyzer **
**     ****Magnetic Wave Complex **
**     ****Magnetometer **
**     ****Energetic Particle Telescope**
**     ****Neutron Detector**
**     ****Radio Spectrometer Detector **
**Mass: 100 kg   ******** Power: 100 W   ******** Telemetry: 100 kb/s**** **

**INTERHELIOPROBE**

**Notes:**

Полезная нагрузка состоит из двух блоков. Это приборы для наблюдений Солнца и приборы для локальных измерений, которые здесь перечислены. Прообразами многих приборов являются приборы, которые использовались в успешно реализованных проектах.

Payload consists of two blocks. These are devices for observations of the Sun and devices for local measurements, which here are listed. Prototypes of many devices are devices, which were used in successfully realized projects.

## INTERHELIOPROBE in Aphelion

**Notes:**
КА в афелии. Солнечные панели полностью раскрыты.

## Interhelioprobe  &  Solar OrbiterRSA              &          ESA2014

**Contact: Prof. Kuznetsov, IZMIRAN**
**kvd@izmiran.ru**

**Interhelioprobe  &  Solar Orbiter****RSA              &          ESA****2014**