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HINODE Operation Plan (HOP)

accepted on

22-mar-2018


 HOP No.

 HOP title

HOP 0351

Coordinated Observations with X-ray spectrometer onboard the SDO/EVE calibration rocket launch

plan term

2018/06/18-2018/06/18

@ @

proposer

 name : Moore, Woods, Caspi, Warren, Ugarte-Urra @  e-mail : Christopher.s.moore[at]cfa.harvard.edu, Christopher.moore-1[at]colorado.edu, tom.woods[at]lasp.colorado.edu, amir[at]boulder.swri.edu, harry.warren[at]nrl.navy.mil, ignacio.ugarte-urra.ctr.sp[at]nrl.navy.mil

contact person in HINODE team

 name : Mariska, Warren @  e-mail : jtmariska[at]gmail.com,harry.warren[at]nrl.navy.mil

 abstract of observational proposal
Main Objective:
Perform Quiet Sun (QS) and/or Active Region (AR) differential emission measure (DEM) and elemental abundance analysis using the X-ray spectrometer (Rocket-3-X123) onboard the SDOEVE sounding rocket underflight, Rocket-EVE EUV spectra, Hinode-XRT X-ray images, Hinode-EIS EUV spectra (if available), and SDO-AIA EUV images.

Scientific Justification:
The SDO-EVE sounding rocket flight currently scheduled for June 12, 2018 at 1 PM MDT (7 PM UT), will contain an X-ray spectrometer to perform solar measurements from ~0.6 . 4 keV with a resolution of E ~ 0.1 keV at 2 keV. This is a great opportunity to conduct spectrally resolved measurements in between the MinXSS-1 (deorbited on May 2018) and MinXSS-2 (scheduled to launch no-earlier-than July 2018) CubeSats missions. Just as important is the opportunity to obtain spectrally resolved ( ~ 1 nm) EUV measurements from ~6 . 137 nm from the scheduled Rocket-EVE observations. These soft X-ray and EUV spectrum are ideal for constraining the quiet Sun and active region coronal temperature distributions and determining the elemental abundance variation from photospheric estimates. Both are vital in understanding heating and dynamical processes that occur in the solar corona. Hinode-XRT filter images will aid in the high temperature plasma constraints and localizing the soft X-ray emission.

Furthermore, the EIS 40h slot full sun raster mosaic data at ~0.1 nm resolution will provide unique images of relatively well isolated spectral lines. These spectral line images allow for direct assessment of the coronal structure at different temperatures, elements and ionization states.
These EIS mosaic and XRT images will be used in analyzing the validity of different coronal heating mechanisms in numerical simulations.

Finally, the composite EUV and soft X-ray spectra, and filter EUV and soft X-ray images and EIS 40h slot mosaic can be compared to the predicted spectrum and spatial emission from full Sun 3D numerical simulations employing various heating methodologies.

Coordinated XRT and EIS measurements a few hours before and a few hours after the SDO-EVE rocket launch on the day of the launch will supply a wealth of data to address numerous questions about the physics and current conditions of the corona.

In summary our objectives are:

1. Construct DEMs from Rocket-3-X123, Rocket-EVE, Hinode-XRT, Hinode-EIS (if available) and SDO-AIA.

2. Asses the validity of current coronal heating models in full Sun 3D numerical simulations by comparison to the simultaneous EUV and soft X-ray spectrally resolved measurements.

 request to SOT
None

 request to XRT
We desire as many full sun (synoptic), sun centered images taking by XRT during the 1 . hour SDO-EVE rocket launch window (#3). Sets of images for #1, and #4to be taken as stated in the DATES section We request the following filters below.

-Al filters give estimations of spectral contributions mostly between 0.7 . 1.6 keV.
*Medium_Al*(short, medium and long exposures to increase dynamic range)
*Thick_Al*(*short if needed*, medium and long exposures to increase dynamic range)
*Thin_Be* is critical!!, This give a similar photon energy response to the Rocket-3-X123 x-ray.
(short, medium and long exposures to increase dynamic range)
*Medium_Be* is critical!!, This give a similar photon energy response to the Rocket-3-X123 x-ray.
(short, medium and long exposures to increase dynamic range)
Thick_Be (long exposure time for a signal check)
*Al_Poly* (short, medium and long exposures to increase dynamic range)Al_Mesh (short, medium and long exposures to increase dynamic range)
Dark . (3 exposures)

Bin all full sun images 2x2.
* = critical for analysis

 request to EIS
If EIS is availablec As of 3/7/2018 Hinode EIS was still powered off.
For details see HOP 130. A summary is below.

EIS study acronym: FULL_SUN_SLOT_SCAN_2
TARGET: Full Sun (multiple pointings)
EXPOSURE TIME: 20s
RASTER: Scanning
SLIT: 40"
FOV: 488"x512"
DATA COMP: JPEG85
DURATION: ~4h (5.75 min/exposure + pointing stabilization+SAA avoidance, 26 exposures)
DATA VOLUME: 364MB (14MBits/exposure, 26 exposures)
SPECTRAL WIND.: 13
LINES: He II 256.3, Si VII 275.3, Fe VIII 185.2, Fe XI 180.4, Si X 258.42, S X 264.2, Fe XII 195.1,
Fe XIII 202.0,
Fe XIII 203.8, Fe XIV 211.36, Fe XIV 274.24, Fe XV 284.1, Fe XVI 262.9
Pointing
|15 spacecraft pointings covering full disk. Two EIS pointings per spacecraft pointing: top and bottom of CCD in order to maximize area and minimize spacecraft pointings|This is a complex observation so for full details please check PDF file (hop_130_vX.X.pdf) at
SolarSoft directory: $SSW/hinode/eis/idl/atest/ugarte

Email Ignacio Ugarte Urra at ignacio.ugarte-urra.ctr.sp@nrl.navy.mil with any specific questions

 other participating instruments
Possible NuSTAR coordinated observation.

 remarks
Dates: We desire two sets of XRT observations on the day of the SDO-EVE rocket launch and one set of EIS observations, on the SDO-EVE rocket launch day (tentatively scheduled for June 12, 2018 at 19:00:00 UT, we will confirm the launch date and time in early June 2018)

Top priority:
Measurements on the SDO-EVE rocket launch day. These measurements are:

1. One set (groups of exposure types, e.i. *short* + medium + long) of synoptic full sun XRT images with each filter (with the filters and exposure types stated in the XRT section) approximately 1 -2 hours before the launch window.

2. During the 1 hour launch window. Synoptic full sun XRT filter images (as stated in the XRT section). As many exposures as possible.

3. Repeat of #1. One set (groups of exposure types, e.i. *short* + medium + long) of synoptic full sun XRT images with each filter (with the filters and exposure types stated in the XRT section) approximately 1 -2 hours after the launch window.

4. EIS full sun raster as stated in HOP 130 (duration ~ 4 hours). To begin approximately 2 . 6 hours after the launch window.

Time window: Short interruptions are OK for ten minute synoptic observations for all the observations stated in the previous section. It is desired that #3 is uninterrupted. Details are in the previous section.

For XRT requests: Email either Christopher.s.moore at cfa.harvard.edu or Christopher Moore at Christopher.moore-1 at colorado.edu

For EIS requests:
Pointing
|15 spacecraft pointings covering full disk. Two EIS pointings per spacecraft pointing: top and bottom of CCD in order to maximize area and minimize spacecraft pointings.
|This is a complex observation so for full details please check PDF file (hop_130_vX.X.pdf) at SolarSoft directory: $SSW/hinode/eis/idl/atest/ugarte

Email Ignacio Ugarte-Urra at ignacio.ugarte-urra.ctr.sp@nrl.navy.mil with any specific questions.

Duration:
|~16min at each pointing.
|~4h total with no gaps.

SAA-free period preferred to minimize duration and facilitate planning. Other periods are OK.

Previous HOP information:
I have submitted HOP 0301 and 0325. Data from HOP 0325 are being written up for a publication on the cross-calibration between XRT and the MinXSS-1 CubeSat.

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