four slit/slot selections available euv line spectroscopy - slits

10
Four slit/slot selections available EUV line spectroscopy - Slits - 1 arcsec 512 arcsec slit - best spectral resolution - 2 arcsec 512 arcsec slit - higher throughput EUV Imaging – Slots Overlappogram; velocity information overlapped 40 arcsec 512 arcsec slot - imaging with little overlap 250 arcsec 512 arcsec slot - detecting transient events Slit and Slot Interchange

Upload: kiara

Post on 07-Jan-2016

27 views

Category:

Documents


0 download

DESCRIPTION

Slit and Slot Interchange. Four slit/slot selections available EUV line spectroscopy - Slits - 1 arcsec  512 arcsec slit - best spectral resolution - 2 arcsec  512 arcsec slit - higher throughput EUV Imaging – Slots Overlappogram; velocity information overlapped - PowerPoint PPT Presentation

TRANSCRIPT

Page 1: Four slit/slot selections available EUV line spectroscopy - Slits

• Four slit/slot selections available

• EUV line spectroscopy - Slits - 1 arcsec 512 arcsec slit - best spectral resolution - 2 arcsec 512 arcsec slit - higher throughput

• EUV Imaging – Slots – Overlappogram; velocity information overlapped– 40 arcsec 512 arcsec slot - imaging with little overlap– 250 arcsec 512 arcsec slot - detecting transient events

Slit and Slot Interchange

Page 2: Four slit/slot selections available EUV line spectroscopy - Slits

EIS Field-of-View (FOV)

360

512

EIS Slit

Maximum FOV for raster observation

512

900 900

Raster-scan range

Shift of FOV center with coarse-mirror motion

250 slot

40 slot

512

Page 3: Four slit/slot selections available EUV line spectroscopy - Slits

The first 3 months….

• Flare trigger and dynamics: Spatial determination of evaporation and turbulence atial determination of evaporation and turbulence in a flarein a flare

• Active region heating: Spatial determination of the velocity field in active region patial determination of the velocity field in active region loopsloops

• Quiet Sun and coronal hole boundary: Determination of the relationship etermination of the relationship between different categories of quiet Sun events.between different categories of quiet Sun events.

The observing time will be split evenly between the topics. If there is an active region we will track it otherwise we will observe quiet Sun and

coronal holes for long periods of time (at least 12 hrs). When there is an active region we will track it, and if there is highly sheared

magnetic field then we will go into flare trigger mode to respond to XRT's trigger. If there are no active regions but there is a quiet prominence we concentrate on this.

Page 4: Four slit/slot selections available EUV line spectroscopy - Slits

Active Regions

• connect the photospheric velocity field to the signatures of coronal heating. This will allow us to determine the dominant heating mechanism in active regions, and will be extended to other coronal brightenings.

• search for evidence of waves in loops and make use of observations for coronal seismology

• study dynamic phenomena within active region loops.

Page 5: Four slit/slot selections available EUV line spectroscopy - Slits

Quiet Sun• link quiet Sun brightenings and explosive events to

the magnetic field changes in the network and inter-network to understand the origin of these events.

• determine the variation of explosive events and blinkers with temperature.

• Search for evidence of reconnection and flows at junctions between open and closed magnetic field at coronal hole boundaries.

• Determine the impact of quiet Sun events on larger scale structures within the corona.

• Determine physical size scales using density diagnostics.

Page 6: Four slit/slot selections available EUV line spectroscopy - Slits

Solar Flares

• determine the source and location of flaring and identify the source of energy for flares. EIS will measure the velocity fields and observe coronal structures with temperature information. Hence will allow us to address the trigger mechanism.

• detection of reconnection inflows, outflows and the associated turbulence which play the pivotal role in flare particle acceleration.

Page 7: Four slit/slot selections available EUV line spectroscopy - Slits

Coronal Mass Ejections

• determine the location of dimming (and the subsequent velocities) in various magnetic configurations allowing us to determine the magnetic environment that leads to a coronal mass ejection.

• The situations to be studied include filaments, flaring active regions and trans-equatorial loops.

Page 8: Four slit/slot selections available EUV line spectroscopy - Slits

Large Scale Structures

• determine the temperature and velocity structure in a coronal streamer

• determine the velocity field and temperature change of a trans-equatorial loop, and search for evidence of large-scale reconnection.

• Using a low-latitude coronal hole, search for evidence of the fast solar wind.

Page 9: Four slit/slot selections available EUV line spectroscopy - Slits

Information is maintained on our website;http://www.mssl.ucl.ac.uk/www_solar/solarB/

The EIS science planning guide shows details of the 3 month plan studies including line choices, which slit/slot, FOV etc.

These studies can be used as a basis for your own studies, or you can make your own.

Page 10: Four slit/slot selections available EUV line spectroscopy - Slits

Data Policy

• The observations recorded during the first six months of operations, which includes the commissioning phase and initial operations, will be released at the end of six months. This period of restricted data release is designed to allow the instrument team’s adequate time to implement and test the data processing and dissemination systems. Limited blocks of data will be released to provide the wider scientific community with an opportunity to interface with the database and to provide feedback to the Solar-B team prior to the full release of data.

• After the first six months all observations will be made available to the scientific community as soon as they are received and processed at ISAS.