SOTSP: HOP 285 Helioseismology
2015-05-27T09:05:00 to 2015-05-27T16:15:30
Science Goal: Multi-height helioseismology of quiet-Sun and active regions. Coordinated observations with VTT
Program: Fast map 82x82", 1 side Q75
Target: Active Region
xcen=-59 ycen=-40
Instrument: SOTSP
HOP/JOP: 285
Description:
Request to SOT HOP Number 0285 BFI (CaII H) 56" x 112" /60sec BFI (G-Band) 56" x 112" /60sec NFI (NaI IV) 82" x 82" /60sec Other Instruments: IRIS: ?gSit-and-stare?h SJI the maximal FOV of an instrument 175 x 175 arc sec. The temporal cadence of the measurement should be not smaller than 10 sec and not larger then 30 sec Spectral lines: SJI imaging data taken for the chromosphere simultaneously. (Mg II H 2803A and Mg II K 2796 A) and transition region (C II 1334/1335A and Si IV 1394/1403A) and one context photospheric pass band (2830 A) Scientific Objectives: The main goal of observing proposal it to plan coordinated multi-wavelengths observations between the IRIS and Hinode space observations, and the Vacuum-Tower and
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Telescope (VTT) located at the Teide Observatory in Canary Islands. Combined measurement between the space IRIS and Hinode, and the recently developed 2D Fabry-Perot HELLRIDE instrument installed at VTT will allow us to obtain the high cadence (60 sec) multi-height imaging observations of solar oscillations from the photospheric level to the corona of the quiet-Sun and active region. The HELLRIDE data provide unique Doppler shifts information simultaneously in 16 bands in and above the photosphere level. This kind of observations will help to understand the propagation of the acoustic waves through the solar atmosphere. The proposed VTT-IRIS-Hinode joined measurements will be the second observing campaign using the HELLRIDE for a thesis work of A.Wisniewska (KIS, Freiburg) focusing on the topic: ?eAnalysis of kinematic energy transfers within the solar atmosphere at high temporal and spatial resolution?f. The observing program would involve at least 10 spectral lines observed simultaneously at medium cadence (30 - 60 sec). FOV instrument is 100 by 100 arc sec and measured with 1k by1k camera. By the image size 512x 512 pixels we obtain the spatial resolution of 0.2 arc sec/pixel. Observations would cover 10 hours each on multiple days to achieve best signal-to-noise performance and to compensate for statistical fluctuations in wave excitation with time. We would make use of the capability of HELLRIDE to switch between wavelength bands at high speed. The range of the spectral lines will cover the photosphere with (Fe I 6173 A) up to the lower chromosphere (H alpha 6562 A). The 10 spectral lines will be selected in such a way to probe the solar atmosphere with the intervals of about 300 km. Therefore we would like to complement out measurement with the Hinode, and IRIS data covering the higher regions of the solar chromosphere, with possible higher cadence. Observations would ideally cover 10 hours each on multiple days to achieve best signal-to-noise performance and to compensate for statistical fluctuations in wave excitation with time. We would make use of the capability of HELLRIDE to switch between wavelength bands at high speed making use of the HELLRIDE property of observing large numbers of spectral lines. The program is planned for observations at the disk center. The target of measurement will be a quiet-Sun region, and an active region (including plage, pore or sunspot).
