EXPECTED SCIENTIFIC OUTCOME from TESIS

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EXPECTED SCIENTIFIC OUTCOME from TESIS

• A.M.URNOV and TESIS Team

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  ?) ? ?? ????????????? ? ?????? ????
  (????????????) ???????? ??????, ????????? ?
  ????????? ?????????? ?????? ? ?????????? ????
• - ????????? ??????? ?????????? (?????????
  ????????)
• - ????????? ??????? ?????? ? ?????????
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• - ??????????? ????????? ? ?????????? ?????????
• - ?????????? ?????????? ??????? ???????
  ??????????
• ?? ?????? ?????? ?????????? (???????????)

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• - ???????????? ?????????? ?????????? ???????????
  ???????? ??????? (??), ????? ?????, ???????????
  ???????????, ????????????, ???????????????
  ???????? 1 5 ???. ???? ? ???????? ????? 1
  30 ?????
• - ???????? ??????? ?????????? ??????? (??),
  ??????????? ??????? ???? (???) ? ??????
  ?????????? ???????? (??), ???????????????
  ????????? 0.1 2 ??? ???? ? ???????? ????? 10
  ??? 10 ?????

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???? ???????????, ????????????? ???????? ??????
????????? ??????

• ????????????? ???????? (???????? ? ??????????
  ???) ? ???????????? (y(T))
• ???????????????-????????? ???????? ???????????
  ??????????? (T(r))
• ???????????????-????????? ???????? ???????????
  ????????? (ne (r))
• ???????????????-????????? ???????? ???????
  ??????? ???????? ????????? (?????? ?????? nz)
• ?????? ????????? ? ??????????? ??????????
  ???????????? n(E)
• ??????? ????????????? ?????????? (???????????
  ?????????) ? ??????????? ?????????? ????????????
  F(v)
• ??????????? ?????? ?????????? ??????

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Golden Age of Solar Physics from Space

• Yohkoh (1991 - 2001) Japan / US / UK
• Hard and Soft X-ray Imaging
• X-ray Gamma-ray Spectroscopy Flares
• SoHO (1996 - ) ESA / NASA
• Solar Heliospheric Imaging
  Helio-seismology
• TRACE (1998 - ) NASA
• Highest Spatial Resolution UV EUV Imaging
• CORONAS-F (2001 - 2005) RSA
• Coronal Imaging and Spectroscopy
• RHESSI (2002 - ) NASA / other
• High-Energy Solar Spectroscopic Imager
  Flares
• CGRO, Ulysses, and other heliospheric missions

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The corona is full of magnetic features!
Twisted Loops
Cusps
S-shaped interconnecting loops
All change with time.
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LDE flares with a growing cusp structure.
Higher temperatures (20 MK) at the outer
edge. Upward motion (plasmoid) in the outer
structure.
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LDE flares with a growing cusp structure.
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LDE flares with a growing cusp structure.
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Flaring Loop and the Surroundings
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Yohkoh canonical view Magnetic reconnection
Rec. point
Rec. ouflow
Shock front
HXR source
Energetic el.
SXR bright loop
Evaporation
HXR sources
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MgXII IMAGING SPECTROHELIOMETERtemperature
response

• Tmin about 4 10 6 K
• Tmax ... 10 7 K

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MgXII IMAGING SPECTROHELIOMETERgoals of
observations

• Monochromatic imaging of coronal plasma with Tgt
  4 MK

• How does the high temperature plasma distribute
  in the solar corona?

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MgXII IMAGING SPECTROHELIOMETERgoals of
observation

• Above loop top heating of coronal plasma during
  solar flares

• What are the reasons of fast heating of coronal
  plasma during solar flares?
• What is the plasma density and temperature in
  the region of above-loop-top heating?

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MgXII IMAGING SPECTROHELIOMETERgoals of
observation

• Plasma heating within cusp-like structures in
  the solar corona

• Can we find the evidence of magnetic
  reconnection through the observation of hot
• plasma dynamics within the large-scale
  cusp-like structures?

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MgXII IMAGING SPECTROHELIOMETERgoals of
observation

• Giant long-life coronal structures of hot plasma
  with T10 MK

• Are the long-life hot structures an apparent
  feature of continuous non-flare particle
• acceleration in the corona?
• Can we derive the rate of the acceleration from
  observations of these structures?
• May this acceleration be a key to the coronal
  heating problem?

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EUV SPECTROHELIOMETER goals of observations

• Determination of plasma temperature composition
  in the solar atmosphere

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????????????????? ??? (285-335A)
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XUV spectroheliograph provides

• The distribution of electron density over the
  temperature
• The distribution of the DEM over the temperature
  and the height
• Diagnostics of thermal/supra-thermal regions
• Diagnostics of elemental abundances

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Density diagnostics
Density sensitive ratios Fe XIII T 1.6
MK 203.80203.82/202.04 321.40/320.81 312.87/321
.40 318.13/321.40 Fe XV T 2 MK
307.75/324.98 284.16/307.75 327.03/307.75 S
XI T 2 MK 291.58/285.82 291.58/281.40 S XII T
2 MK 288.42/299.54
Diagnostics is based on CHIANTI
(http//www.solar.nrl.navy.mil/chianti.html).
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Average density diagnostics
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??? ??? ???????? ??????? ? ???????
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???? 12.11.2001(Mg)
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????????????? ????????????? ???
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2001, November 12
SXT
SPIRIT MgXII
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2001, November 12
1
1
1
SXT
MgXII
ALL
1
SXT SPIRIT
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SXTMg, 12.11.2001 (Height)
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SPIDER (IATMg) 29.12.2001
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Height distribution of line intensities
(29.12.2001)
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??????? 10 ?? ?????? ? ??????? ??????(MgXII
8.42?)
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???????? ?????????????? ??????? ?????????
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????????? ??????? ????????? ?????????
??? ?????
33
?????? ?????
34
?????? ?????
35
????????? ?? ? ??? ???????
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????? ????????? ? ??????? 28 ??????? 2003 ????

???????? ? ?????????? ??????? 28/10-2003,
110139 UT ?) ????? ????????? ?
?????? 175 Å ????????? ?????? b) ???????
????????????? ? ???????? ????????? 1, 2 ? 5 c)
??????? ????????????? ???? ??????? ????????? ?
??????? ?????? 175 Å ? EIT 195 Å, ?????????? ?
?????? ????????????? ????? ?? ??????? d)
?????? ????? ?? ?????? ? ?????? GOES 1-8 Å.
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??? ???????? ??????? ? ?????????

???????? ????????????? ??????? ? ????????
????????? ? ?????????? ??????? (304 Å) ? ??????
(175 ? 195 Å) ? ??????? 17-18 ?????? 2003 ?.
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METHODS OF TESIS OBSERVATIONS

• Multi-wavelength simultaneous observations of
  full Sun in 4 spectral channels

MgXII 8.42 A
FeXX 132 A
TESIS will provide simultaneous imaging of the
Sun in 4 spectral channels, including EUV channel
295-315 A, which allows to derive the density and
the temperature composition of the plasma.
EUV 295-315 A
HeII 304 A
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THANKS FOR ATTENTION