Proposed SOOP Coordinators
Radoslav Bucík, Davina Innes, David Berghmans, Susanna Parenti, Don Hassler, A. De Groof, A. Zhukov
Description
Tracking a complex AR of the Sun, for AR dynamics or tracking of a region for initiation. Making use of Solar Orbiter's higher resolution capabilities, so would be at the best resolution (no binnings).
The acceleration mechanism in solar flares, tremendously enhancing (up to factors of ten thousand) rare elements like 3He and ultra-heavy nuclei, has been puzzling for almost 50 years (e.g., Mason 2007; Reames 2017). The goal of this SOOP is to examine in detail underlying photospheric sources of these so-called 3He-rich solar energetic particles (SEPs).
Specifically, the SOOP addresses the following two problems (References at bottom of this page):
1) Does the magnetic flux emergence (cancelation) play a fundamental role in energetic particle production and release from the Sun? What is the growth rate of ARs associated with 3He-rich SEPs (e.g., rapid growth may imply high intensities/enrichments, shorter time to SEP production/release)? Statistically, the 3He-rich SEP sources (regions to which we are connected from the Earth) are located near the west limb (~W55). Due to a projection effects this science question cannot be properly investigated with NEO based observations. Though STEREO-A was in the right position having a direct view on 3He-rich SEP sources, it does not provide surface magnetic field data. Approaching to the Sun the SO connecting point move towards the Sun-SO line, improving magnetic field observations of the connected regions (Bucik et al. 2014; Chen et al. 2015).
2) Would we detect 3He-rich SEPs from frequent small emerging bipoles (although without significant EUV flaring as speculated by Wang et al. 2006) at closer distances to Sun? The SO will be able to detect the events with much smaller intensities than at 1 AU (at perihelion, a factor of ~ 50 if applying a simple inverse cube scaling law) probably allowing their detection also during solar minimum conditions. Thus, with SO we may see 3He-rich SEPs from new sources.
[source: SOL-PHI-MPS-MN5100-TN-2, description updated by Andreas Lagg (email 10 Apr '17)]
Default SOOP duration: 1 day
Pointing requirements: target tracking
Triggers: enabled
| Instrument | Mode | Comment |
|---|---|---|
| EUI | FSI Synoptic mode (S) and EUV & LYA Active Region modes (A) | Will need triggers to manage TM. Model flush volume as 2500MB (~1hr event+FSI) This SOOP is looking for eruptive events in HRI. However, if no eruptive event is observed, then one can download one hour of data and that would be sufficient for a fine scale structure study. |
Metis | May contribute if disk-centre pointed (not modelled for now) | |
| PHI | PHI_nominal_HRT_0 + PHI_magnetograph_HRT_2 (3 quantities) for context around 'event' | Model flush volume as 850MB (~1hr event + rest in mode 2) |
| SPICE | Use observation called SPICE_CME_COMP in modelling. | |
| STIX | STIX Normal Mode | Triggers Active |
| SAP objective | Target | Duration | Opportunity (e.g., orbital requirements, solar cycle phase, quadrature ...) | Operational constraints | Additional comments |
|---|---|---|---|---|---|
| 2.1.1.1 CME initiation | Active Region | 2 days | Earth side (≤ 60°), All phases of the solar cycle, perihelion | In RSW RSW Extention needed for target selection VSTP needed for target updated Offpointing so no Metis | |
| 2.1.1.2 CME structure | Active Region | 2 days | Earth side (≤ 60°), All phases of the solar cycle, perihelion | In RSW RSW Extention needed for target selection VSTP needed for target updated Offpointing so no Metis | |
3.1.2.1 Understand energy release and particle acceleration process | Active Region Properties of flare energy release Acceleration relating to the magnetic reconnection process | Statistics (Limited by EUI internal memory) | Perihelion preferred. Best when co-temporal images from Earth are available | Target tracking | EUI/HRI 1 min cadence over several hours for flare with direct connection to SolO. To be done together with I_DEFAULT |
| 3.1 How and where are energetic particles accelerated at the Sun? [source: SOL-PHI-MPS-MN5100-TN-2] | ARs | several days | perihelion | co-observations fro Earth | |
5.5 Additional Science Objectives of PHI: 5.5.2.5 How do magnetic fields emerge on the solar surface? [source: SOL-PHI-MPS-MN5100-TN-2] | emerging flux regions | PHI cadence may need to be higher in QS (2-5 minutes) than for ARs (5-10 mins) | |||
| 3.1.2.0 Impulsive SEP event sources |
References
Bucik R., Innes D.E., Mall, U. et al. 2014, ApJ 786, 71
Chen N.-H., Bucik R., Innes D.E., Mason, G.M. 2015, A&A 580, A16
Mason G.M. 2007, SSRv 130, 231
Reames D.V. 2017, Solar Energetic Particles, Lecture Notes in physics 932, Springer
Wang Y.-M., Pick M., Mason G.M. 2006, ApJ 639, 495
2 Comments
Yannis Zouganelis
In principle this is not a remote-sensing only SOOP since EPD is needed for the goal relative to the 3He-rich SEPs.
Anik De Groof
SOOP ID in SOOP Kitchen = RS1