HOP 0223

HINODE Operation Plan (HOP)

accepted on

18-oct-2012

HOP No.

HOP title

HOP 0223

The origin of high speed mass flows in solar polar regions

plan term

proposer

name :

Goode

e-mail :

pgoode[at]bbso.njit.edu

contact person in HINODE team

name :

Tarbell

e-mail :

tarbell[at]lmsal.com

abstract of observational proposal

The solar polar regions are filled with small scale activity, like plumes and X-ray jets.
Such activity is accompanied by mass flows with speeds of tens of kilometers per second. High-speed solar wind is believed to be associated with these various small scale activities. Despite many space-based observations from SOHO and Hinode, the exact location of these small scale activities in the photosphere is still unknown. High resolution He I 10830 imaging with NST at BBSO has provided us an unprecedented opportunity to observe mass flows from the photosphere (Ji, Cao and Goode, 2012, ApJ, 750, 25). NST's AO system is able to lock on granulation for several hours during a day of good seeing. Targeting solar polar regions with the NST's high resolution He I 10830 imaging will enable us to observe these small scale manifestations of solar activity. Simultaneous observation in broad band TiO will allow us to track convective motion of the granular field and changes in features in the inter-granular lanes. SOT provides us an excellent opportunity to study the variation of small-scale magnetic features, which have been suggested as drivers of the outflow. EIS would observe the flow field in the corona through spectroscopic scanning.

request to SOT

SOT/FG
SOT/FGIV Stokes I and V images with a field of view of 164"x164" and a cadence of ~30 seconds in Fe I 5250.2 to obtain line-of-sight magnetograms and intensity images of the photosphere.

request to XRT

Filter : Al/Poly with FOV : 128"x128" with 1x1" resolution and 1 minutes cadence.

request to EIS

EIS FOV is centered on the SOT FOV. The main aim of EIS is to measure the velocity of the million degree hot mass flow accompanying the small-scale activity.
*2" slit scan
*FOV 100"x256"
*40 sec exposure time
*Lines: He II, O V, Si VII, SiX, Ca XVII, Fe VIII X,XI,XII,XIV,XVI, XXIII

other participating instruments

The BFIs at the New Solar Telescope (NST) and adaptive optics (AO) in Big Bear Solar Observatory, CA, USA. BFIs will follow a same target region on each day, with HeI 1083 nm, Ha and TiO 706 nm (90" x 90" FOV, 5-10 sec cadence).

remarks

-- The longitudinal magnetic component has the highest priority.
-- We will use simultaneous AIA/SDO and HMI/SDO observations.