Instrument

SPICE

Flare ribbon watch:

Sit and stare observation with a 1-5 sec cadence

Other possibility for a different instance (oriented towards CME watch):
SPICE Dynamics mode. 15 lines (2 profiles, 13 intensities)

Spectral window in and around:
Lyman Beta and O VI (1020-1050 Å), Lyman gamma 973 Å, C III 977 Å, Fe XX 721.6 Å.

Centre of raster at centre of EUI. Stepping 4” instead of 2” is another possibility. A CME watch could be added after N repeats of this SOOP (∼45 minutes, 4” resolution).

EUI HRI

HRI in highest spatial resolution. HIGH CADENCE: 3-10 seconds. Only HRIEUV in highest spatial resolution, HRILYA in 2x2 binned.

Will limit telemetry for entire orbit. 

EUI FSI

FSI 174 (adapted) Synoptic mode (S), MEDIUM CADENCE: ~3 minutes. FOV: FULL (no rebinning)

The FSI images allow to study potential EUV waves associated with the flare. Lowest level of support is FSI only.

STIX

STIX Normal Mode

Trigger, high cadence light curve, location

PHI

PHI science mode 2 (FDT); burst mode triggered by STIX to catch white light flare in high cadence

Observations used for context and extrapolations.

SWA

SWA Normal Mode with SWA trigger on

In situ solar wind signature of potential CME associated with the flare, can it be triggered by STIX.

MAG

MAG Normal Mode with MAG trigger on

In situ magnetic field signature of potential CME associated with the flare.

EPD

EPD Normal Mode with EPD trigger on

In situ particles signature of potential SEP associated with the flare.

SoloHI

SoloHI Normal mode

Heliospheric imaging of potential CME associated with the flare.

RPW

RPW Normal Mode with RPW trigger on

Remote sensing will provide observations of shock drivers, such as flares (location, intensity, thermal/non-thermal electron populations, time-profiles), and manifestations of CMEs (waves, dimmings, etc.) in the low corona with a spatial resolution of a few hundred kilometers and cadence of a few seconds.

• Origin from the footprints of newly formed loops (Hurford et al., 2006).

• Acceleration relating to the magnetic reconnection process.

• Properties of flare energy release (in high spatial and temporal resolution).

For the magnetically well-connected 2 November 2003 and 20 January 2005 flares, the spectra inferred for the energetic protons that produce the X-ray lines observed by RHESSI are essentially the same, within measurement uncertainties, as the spectra of SEP protons at 1 AU. The extremely rapid rise of SEP fluxes at 1 AU after the 20 January 2005 flare X-ray peak raises serious questions about CME-driven shock acceleration. Measurements of SEPs close to the Sun will provide the timing and compositional information to evaluate how significantly do large flare contribute di- rectly to gradual SEP events.

Prompt events are well correlated with the occurrence of 3He rich SEP events. However, arrival time studies of ions seen at 1 AU suggest a delayed release of the ions relative to electrons, at least when assuming scatter-free transport. This is rather puzzling as it suggests a different accelerator for electrons and ions despite the closely connected occurrence. However, electrons and ions could still be released simultaneously with propagation effects explaining the observed delays. This objective is about exploring if the comparative delay is real or due to propagation effects. It should be studied in different heliocentric distances and hopefully near the perihelion in order to better establish the nature of the flare region (with STIX & EUI). Complete set of observations is required: STIX, EUI, RPW + ground-based radio observations (good to have). That will allow studying the magnetic structures along which flare-accelerated particles escape into interplanetary space.

5.1 Additional Science Objectives of EUI.

5.1.1 

Study the corona and its phenomena in a high spatial and temporal scale (active regions during flares or in quiescent conditions, coronal holes, quiet Sun)

Whatever the active region target, the high spatial resolution of HRI is used in a mode close to A mode with a time resolution of the order of 1 sec. For the polar coronal hole mode, the high latitude is mandatory and the compression in Lalpha possibly lower than 15 (mode C). Complementary observations of SPICE in Lbeta would be very useful.