ESA/NASA Mission Solar Orbiter

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Nov 16, 2013 (3 years and 11 months ago)

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The involvement of PMOD/WRC in the

EUI and SPICE instruments onboard the

ESA/NASA Mission Solar Orbiter


Haberreiter
, Margit
;
Schmutz
, Werner
;
Gyo
, Manfred; B
üchel Valeria, Dürig Fabian;
Pfiffner,
Dany;

in collaboration with Swiss Industry and the Solar Orbiter Team


Physikalisch
-
Meteorologisches

Observatorium

Davos

and World Radiation
Center

(PMOD/WRC)
,
Davos
,
Switzerland


Margit.Haberreiter@pmodwrc.ch



Synthetic Spectra as calculated with the SOLMOD code (
Haberreiter

2011, 2012) showing the spectral ranges at
which EUI (left panel) and SPICE will observe. EUI will take images in the EUV at 17.1 nm and 30.4 nm observing
the strong Fe XII 17.1nm and He II 30.4 nm,. SPICE will observe in two spectral intervals, between 703.9
-

790.2
Å and 972.5
-

1049.2 Å, indicated on the right hand panel.














2.
EUI and SPICE Instruments and main Science goals














4.
Science Observations with SPICE and EUI

Figure

2
.

The

EUI

(Extreme

Ultraviolet

Imagers

is

composed

of

two

high

resolution

imagers

(HRI),

one

at

Lyman

α

and

at

17
,
4

nm

one

dual

band

full
-
sun

imager

(FSI)

working

alternatively

at

the

two

17
,
4

and

30
,
4

nm

EUV

pass

bands
.

In

all

the

units,

the

image

is

produced

by

a

mirror
-
telescope,

working

in

nearly

normal

incidence
.














Solar Orbiter is an ESA/NASA mission


By approaching as close as 0.28 AU, Solar Orbiter will
view the Sun with high spatial resolution and combine this
with in
-
situ measurements of the surrounding
heliosphere
. Thanks to its unique
orbit (see Figure above,
right panel),
Solar Orbiter will deliver images and data of
the unexplored Sun's polar regions and the side of the
Sun not visible from Earth
.















3.
Components
for
SPICE and
EUI
built and managed by PMOD

Figure 2.
U
pper panel:

The SPICE Door Mechanisms (SDM)

resides at the entrance of the SPICE instrument. It
contains a movable shutter paddle to provide contamination control during ground and launch activities. When the
shutter is closed, it forms a labyrinth seal to form a
purgeable

instrument cavity for contamination protection
during AIT and launch.
L
eft panel:

The off
-
axis parabola mirror forms an image of the sun onto the entrance slit
assembly containing four interchangeable slits of differing widths. The slit selects a portion of the solar image and
passes it to a concave TVLS grating which re
-
images the spectrally dispersed radiation onto two array detectors.

Each slit is fabricated on a single crystal Silicon wafer using precision lithography techniques developed for
electronic chips

Right upper panel:

LVPS

Right lower panel:
EUI optical bench structure.

2.
Solar Orbiter
-

Overview

Table 1:
Key spectral lines as to be observed by SPICE:

References:

Haberretier
, M. 2011,
Solar EUV Spectrum Calculated for Quiet Sun
Conditions, Solar Physics, 274, 473.

Haberreiter, M. 2012,
Towards the reconstruction of the EUV irradiance
for solar Cycle
23. In:
Proceedings of the International Astronomical
Union, IAU Symposium, Volume 286, p.
97
-
100.

Figure

3
.

Overview

of

the

SPICE

instrument
.

Spectrally

resolved

imaging

spectroscopy

allows

us

to

understand

the

mechanisms

responsible

for

flow

of

mass

and

energy

through

the

solar

atmosphere
.

SPICE

is

built

on

the

heritage

from

SOHO/SUMER

and

CDS,

Hinode
/EIS
.

The

goal

is

to

link

SPICE

observations

with

in
-
situ

measurements

onboard

Solar

Orbiter

.

This

will

allow

us

to

link

processes

in

the

solar

atmosphere

with

the

heliosphere
,

in

particular

understand

the

dynamics

in

the

solar

atmosphere

and

the

processes

responsible

for

the

acceleration

of

the

Solar

Wind
.

Two

spectral

windows

will

be

observed

with

a

separate

shortwave

and

longwave

detector
:

Detector 1:


703.9
-

790.2 Å

Detector 2:


972.5
-

1049.2 Å

The Solar Orbiter spacecraft is a Sun
-
pointed, 3
-
axis stabilized
platform, with a dedicated heat shield to provide protection from
the high levels of solar flux near perihelion. Feed
-
throughs

in the
heat shield (with individual doors) provide the remote
-
sensing
instruments with their required fields
-
of
-
view to the Sun. Single
-
sided solar arrays provide the required power throughout the
mission over the wide range of distances from the Sun and can
be rotated about their longitudinal axis to manage the array
temperature, particularly important during closest approach to the
Sun.

The main science goals of Solar Orbiter are:



Determine the properties, dynamics and interactions of
plasma, fields and particles in the near
-
Sun
heliosphere



Investigate the links between the solar surface, corona
and inner
heliosphere



Explore (at all latitudes) the
energetics
, dynamics and
fine
-
scale structure of the Sun’s
magnitized

atmosphere



Probe the solar dynamo by observing the Sun’s high
-
latitude field, flows and seismic waves

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