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HINODE Operation Plan (HOP)

accepted on

22-sep-11


 HOP No.

 HOP title

HOP 0203

Understanding the Driving Mechanisms and Properties of RBEs Using IBIS and Hinode

plan term

2011/10/17-2011/10/23
2012/10/24-2012/11/08
2015/06/08-2015/06/14

@ @

proposer

 name : Deng, Wang @  e-mail : nd7[at]njit.edu

contact person in HINODE team

 name : Shimizu @  e-mail : shimizu.toshifumi[at]isas.jaxa.jp

 abstract of observational proposal
Recent discovery of type II spicules at solar limb (De Pontieu et al., 2007 by using Hinode) and "Rapid Blueshifted Excursions" (RBEs; Langangen et al. 2008 by using IBIS) on solar disc has drawn much attention of solar physicists, mainly because of their rapid heating, high speed upflow only, and potential important role in coronal heating and mass transport for solar wind. However we are still far from fully understanding of their properties and driving mechanisms. More observations are certainly needed for statistical and comprehensive studies of their physical properties in order to understand the underlying driving mechanisms. One of the most promising mechanisms is the magnetic reconnection at small scale. In order to verify this or provide options for alternative mechanisms, we plan to carry out on-disc observations of RBEs using the Interferometric BIdimensional Spectrometer (IBIS) at the Dunn Solar Telescope (DST) in coordination with high resolution and high cadence magnetograms from Hinode SOT/SP and SOT/NFI. We will observe with IBIS using chromospheric H-alpha and Ca II 854.2 nm lines to study the properties (velocity, density, temperature and statistical distribution) of these small-scale ejections. The on-disc magnetic field observations by Hinode allow us to study the geometry and evolution of photospheric magnetic fields associated with these jet-like features so that processes which lead to energy deposition and dissipation, such as flux emergence, convergence, cancellation etc at small scales can be characterized. We also plan concurrent EIS and XRT observations in order to investigate the coronal response, mass and energy outputs of RBEs. We will observe RBEs in different regions (such as active region (AR), plage, inside coronal hole (CH) quiet Sun (QS) and outside CH QS) to study their common and different properties and possible driving mechanisms.

We understand and comply that Hinode team now give priority to AR observations that may produce flares. Since we will also observe RBEs in different regions, if there is an AR that may produce flares, we will choose that AR same as Hinode. When there is no flare-productive ARs on the Sun, we then choose to observe QS. We also allow Hinode to change target during the coordinated observation in case a region is producing flares.

References:
De Pontieu, B. et al. 2007, PASJ, 59, 655-662
Langangen, O. et al. 2008, ApJ, 679, L167

 request to SOT
~1590Mbits/day

Combination of SP and NFI observation. The observing procedure is the same for every day during the coordinated observing run. Only the target will change.

SP: ~400Mbits/hr, 1200Mbits/day
repeat SP IQUV scans (fast map, FOV 110" x 123", 0.32" slit, 20 min cadence) during the coordinated observation. The gaps between SP scans due to the SAA periods are accepted.

FG: ~130Mbits/hr, 390Mbits/day
NFI Na I D 5896 longitudinal magnetograms (MG 4 V/I), cadence 64 sec, in the observing period. Similar to the SP FOV. 2x2 summing.

 request to XRT
~10 Mbits/hr, 30 Mbits/day
Ti/Poly images, FOV 192" x 192" in minimum to completly cover the SOT FOV, 1"-resolution, cadence 1 min, Q=95, run during the coordinated observation. Include G-band exposures in very low cadence for alignment purpose. Full-Sun context at the beginning and end of each day coordinated observing run.

 request to EIS
~43Mbits/hr, 129Mbits/day

We will use EIS Study 421.
OBJECTIVE: Observe the same target region as SOT, to measure flows, electron densities and temperatures in RBEs associated jets.
TARGET: AR, plage, outside CH QS, inside CH QS
NO. OF RASTERS: 1 (repeat the raster scan during the coordinated hours)
POINTING: Better to align the center of EIS's FOV with the centers of FOVs of SP and NFI

EIS Study - 421
ACRONYM BP_response1_2raster
RASTER ID 400
ACRONYM BP_response1
LL_ID 219
RASTER TYPE: SCANNING
NO. OF POINTING POSITIONS: 50
SCAN STEP SIZE (arcsec): 2
NO. OF WINDOWS: 13
WINDOW WIDTHS (pixels): 24,24,32,24,32,24,24,24,24,24,24,24,24
WINDOW HEIGHT (pixels): 128
SLIT/SLOT: 2"
EXPOSURE TIMES (ms): 20000
EXPOSURE DELAY (ms): 0
FOV: 100 x 128
ESTIMATED CADENCE: 17 min
DATA COMPRESSION: DPCM
Line List: FeX 184.54, FeVIII 185.25, FeXII 186.74, OV 192.90, FeXII 195.12, FeIX 197.86, FeXIII 202.04, FeXIII 203.82, HeII 256.32, FeXVI 262.98, MgVI 269.00, FeXIV 274.20, FeXV 284.16

 other participating instruments
The Interferometric BIdimensional Spectrometer (IBIS) at the Dunn Solar Telescope (DST) and adaptive optics (AO) in National Solar Observatory, New Mexico, USA. IBIS will follow a same target region on each day, with Halpha and Ca II 854.2 nm lines (90" x 90" FOV, 5-10 sec cadence, ~27 wavelength points for a full wavelength scan). Parallel G-Band and Ca K imaging channels with FOV of about 120??~120?? and cadence of 1 minute will also be provide by DST.

 remarks
[Time period] 2012/10/24-2012/12/08. Hinode observing support for 3 hours (specified below) per day on 7 consecutive days is desired, while if Hinode changes target to a promising flare-productive AR during the coordinated observing run is also accepted. We will inform the Hinode teams well in advance about the local weather conditions (Contact person: Na Deng, e-mail: nd7@njit.edu, cell phone:  001 818 585 9547 ).

[Time window] For this run we prefer 14:15 - 18:15 UT

[Target] We will follow a same target region on each day, i.e., observations need to compensate for solar rotation. On different days, we may choose different target regions, such as AR, plage, outside CH QS, inside CH QS. We will preferentially select near disc center regions. Na Deng will specify detailed pointing and inform Hinode team every day.




[Time period] 2011/10/17-2011/10/23. Hinode observing support for 3 hours (specified below) per day on 7 consecutive days is desired, while if Hinode changes target to a promising flare-productive AR during the coordinated observing run is also accepted. We will inform the Hinode teams well in advance about the local weather conditions (Contact person: Na Deng, e-mail: nd7@njit.edu, cell phone:  001 818 585 9547 ).

[Time window] The best possible seeings at DST are from 14-17 UT in October. Continuous Hinode observing support in this time window is desired but not required.

[Target] We will follow a same target region on each day, i.e., observations need to compensate for solar rotation. On different days, we may choose different target regions, such as AR, plage, outside CH QS, inside CH QS. We will preferentially select near disc center regions. Na Deng will specify detailed pointing and inform Hinode team every day.

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