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HINODE Operation Plan (HOP)

accepted on


 HOP No.

 HOP title

HOP 0113

Too: Spicule Seismology (AR)

plan term


@ @


 name : Erdelyi, Doyle, Marjarska, Mathioudakis, Jess, Morton, Reardon, Scullion @  e-mail : jgd[at]arm.ac.uk

contact person in HINODE team

 name : Culhane @  e-mail : jlc[at]mssl.ucl.ac.uk

 abstract of observational proposal
The rapid rise of plasma temperature up to 1 MK from the solar photosphere towards the corona is still an unresolved problem in solar physics. It is clear that the mechanical energy of sub-photospheric motions is transported somehow into the upper solar atmosphere, where it may be dissipated leading to the heating of the ambient plasma. A possible scenario of energy transport is that the convective motions and solar global oscillations may excite magnetohydrodynamic (MHD) waves in the photosphere, which may then propagate through the chromosphere carrying relevant energy into the corona.
Spicules are grass-like spiky features best seen in chromospheric spectral lines at the solar limb. Beside the morphological and global dynamic studies there are early observational reports on oscillatory phenomena in spicules. However, only a limited number of studies have addressed spicule oscillations with recent high-resolution ground and space-based observations. It is strongly anticipated that signatures of the energy transport by MHD waves through the chromosphere may be detectable in the oscillatory dynamics of spicules. A comprehensive novel observational study of waves and oscillations in spicules, to the best of our knowledge, is still lacking and such observational campaign could clarify important details of the magnetic coupling from the photosphere to corona.
We plan to use existing Hinode, SoHO & TRACE sequences, in addition to acquiring high-cadence ROSA & IBIS data (weather permitting). What is the relationship between spicules, macrospicules and Jets as seen in the TR and corona? Why are spicules as seen in ARs of shorter duration? Does this imply a different heating mechanism? How do spicules manifest themselves in the TR and corona?

Primary Objectives
The primary objective of this proposal is not only to study the dynamic activity in the lower solar atmosphere but to trace that activity to the TR and corona.

Our observing setup will allow us to identify oscillatory power (via FWHM oscillations) in velocity and intensity with frequencies in excess of 20mHz.  With XRT and EIS, we will acquire images and spectral data to enable a determination of the flow, temperatures and electron density structure in the upper atmosphere.  SOT will provide magnetograms in Na D I, Ca II K and if possible H alpha line center and wing emission.
TRACE will provide high-cadence observations with the 171 A filter. SUMER will provide high spectral resolution for selected transition region lines providing a diagnostic of the flow structure.

 request to SOT
FILTERS:       Ca II H
FOV:            120"x100"
CADENCE:        As high cadence as possible.      
START TIME:     15:00 UT
END TIME:       TBD      
REPETITION:     Repeat to fill the available time slot
XCEN           TBD
YCEN           TBD

FILTERS:        Na I D shuttered IV plus Halpha center and wing(s) if possible
FOV:            220"x164"
CADENCE:        As high cadence as possible.      
START TIME:     15:00
END TIME:       TBD      
DURATION:      3-4 hrs  
XCEN:            around 300 "
YCEN:            around 100"

 request to XRT
FILTERS:       Al/Poly, several  G-band images for coalignment
CADENCE:       ~40 s
FOV:           384"x384"
START TIME:    15:00
XCEN           xcen = xcen(SOT)
YCEN           ycen = ycen(SOT)

 request to EIS
STUDY:           madj_ar
STUDY DURATION:  around 32 min
REPETITION:      run once
FOV:             70"X248"
START TIME:      15:00 UT
END TIME:        TBD
XCEN:            TBD
YCEN:            TBD

STUDY:           madj_ar_small
STUDY DURATION:  around 12 min
REPETITION:      repeat to fill the remaining time slot
END TIME:        TBD
FOV:             24"x248"  
XCEN:            TBD
YCEN:            TBD
Rot. comp.:      Rotation compensation to be applied i.e. feature tracking

 other participating instruments


171 A filter with 1550, 1700, 1600 context images every 30 min.
Rot. comp.:      Rotation compensation to be applied i.e. feature tracking
START TIME:    15:00
Target: Polar region

Sac Peak .. Dunn Solar Telescope

With the DST equipped with ROSA & IBIS we aim to achieve the following:
(a) Full Stokes polarimetry using the magnetically sensitive Fe I line at

(b) Scan individual line profiles. Each scan will last for approximately 3 sec and waves with frequencies up to ~160 mHz will be studied (Nyquist frequency). Lines that may be used include Fe I (7090A) & Ca II (8542A) that are formed in the low photosphere, upper photosphere and chromosphere respectively.

(c) The IBIS observations will be combined with simultaneous ROSA imaging in H alpha, G-band, Ca II k and white light continuum. ROSA imaging at high spatial and temporal resolution will be essential as it will allow us to disentangle any intensity oscillations that may be associated with kink and/or sausage waves modes. We will therefore be in a position to show the unambiguous detection of Alfvenic wave modes that may exist in the lower solar atmosphere.

Requested Observing interval
We request 4 shifts; 28, 29, 30 April & 1 May from 15:00 UT for ~4 hrs. SUMER has allocated for this 28th & 29th April from 14:00 UT - 18:00 UT.

Pointing: Two days in an AR


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