HOP list   Monthly Events

HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0260

Understanding the Formation, Heating, and Initiation of Magnetic Flux Rope

plan term


@ @


 name : Cheng, Li, Ding @  e-mail : lying.nju[at]gmail.com

contact person in HINODE team

 name : T. Watanabe @  e-mail : watanabe[at]uvlab.mtk.nao.ac.jp

 abstract of observational proposal

1: To study the spectroscopic characters of magnetic flux rope, especially prior to its eruption.
2: To find the location of heating of the flux rope.

Magnetic flux ropes are twisted magnetic field line structures. It has been widely accepted that the flux rope is the critical structure of coronal mass ejections (CMEs) that are most energetic events in the solar system and cause severe space weather. Zhang et al. (2012) and Cheng et al. (2013) found that the flux rope shows an elongated EUV channel structure in the AIA high temperature passbands (e.g., 131 A and 94 A). However, where and how the flux rope is heated are unknown. In addition, what is the signature of flux rope in the lower solar atmosphere? And how is the flux rope activated and erupted? These questions are not fully resolved. The high-resolution observations from the three instruments on board Hinode cover the photosphere, chromosphere, and corona, and will shed light on the formation, heating, and initiation of the magnetic flux rope.

 request to SOT
BFI: Ca II H; FOV: 218h x 109h; Cadence: 10 s
NFI: Stokes I/V Fe 630.2 nm; FOV: 328h x 164h; Cadence: 10 s
SP: Stokes I, Q, U, V; FOV: 40h x 164h; Cadence: Fast Map Mode

 request to XRT
filter: thin-Be, FOV: 384h x 384h, Cadence: 10 s

 request to EIS
fast scan: EIS study ID: 464 - Qub_Hi-Cad_Flare_2s-Exp_104hx104h
slit: 2h
Exposure time: 5 sec
Step size: 2h
FOV: 104h x 104h
He II 256.32
O V 192.90
O VI 184.12
Mg VI 268.99
Mg VII 280.75
Fe VIII 185.21
Fe X 184.54
Fe XI 182.16
Fe XII 195.12
Fe XIII 202.04
Fe XIV 274.20/264.79
Fe XV 284.16
Fe XVI 262.98
Fe XVII 254.87
Ca XVII 192.82
Fe XXIII 263.76

 other participating instruments
other participating instruments
IRIS: high-cadence slit-jaw images and spectra in the UV band

| Target of interest: active regions with the possibility of producing flares/CMEs.
| Our observation proposal for BBSO during August 19-24 has been accepted.
| The daily best-seeing observing time at BBSO is from 17:00 UT to 21:00 UT.
| We will use simultaneous AIA and HMI observations.

HOP list   Monthly Events