• Title, Summary, Keyword: chromosphere

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Chromospheric oscillation signatures observed by the NST FISS

  • Kim, Yeon-Han;Cho, Il-Hyun;Bong, Su-Chan;Cho, Kyung-Suk;Yang, Heesu;Park, Young-Deuk
    • The Bulletin of The Korean Astronomical Society
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    • v.38 no.2
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    • pp.92.1-92.1
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    • 2013
  • In this study, we examined chromospheric oscillation signatures in two solar active regions, a limb active region and a sunspot with a light bridge, observed by the Fast Imaging Solar Spectrograph (FISS) of the 1.6m New Solar Telescope (NST) at Big Bear Solar Observatory. The FISS is a slit spectrograph with a fast imaging capability and can observe the solar chromosphere in $H{\alpha}$ and Ca II $8542{\AA}$ bands simultaneously with high spectral resolutions. After dark and flat correction, we compensated for image rotation at the Coude focus and made image alignment. We estimated Doppler shifts over active regions using the bisector method and investigated the temporal and spatial fluctuations of Doppler shifts for some selected cases. And we obtain the power map by using the Lomb-Scargle periodogram technique to examine the oscillation power at different features. Finally, we will discuss our results and implications.

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MULTI-WAVELENGTH FIBRIL DYNAMICS AND OSCILLATIONS ABOVE SUNSPOT WAVE PROPAGATION

  • MUMPUNI, EMANUEL S.;HERDIWIJAYA, DHANI;DJAMAL, MITRA;DJAMALUDDIN, THOMAS
    • Publications of The Korean Astronomical Society
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    • v.30 no.2
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    • pp.59-60
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    • 2015
  • High resolution, multi-wavelength images from the Dutch Open Telescope were used to study the detailed mechanisms that might be involved in the multiple layer solar atmosphere observed in high cadence multi-wavelength observations. With the exceptional data observed for active region NOAA 10789 on 2005 July 13th, we study the changing pattern of the fibril using multi-wavelength tomography of the $H{\alpha}$ line center and blue wing, Ca II H, and the G Band. It is believed that a long fibril that is rooted in the umbra, with longer apparent periodicity, may be due to morphological changes. To determine this, we conduct phase difference and coherency analysis between points along the fibril to understand how the wave propagates.

The Observational Evidence for the Internal Excitation of Umbral Velocity Oscillations

  • Cho, Kyuhyoun;Chae, Jounchul
    • The Bulletin of The Korean Astronomical Society
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    • v.43 no.2
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    • pp.47.2-47.2
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    • 2018
  • The umbral oscillations of velocity are commonly observed in the chromosphere of a sunspot. Their sources are considered to be either the external p-mode driving or the internal excitation by magnetoconvection. Even though the possibility of the p-mode driving has been often considered, the internal excitation has been rarely investigated. We report the observational evidence for the internal excitation obtained by analyzing velocity oscillations in the temperature minimum region of a sunspot umbra. The velocity oscillations in the temperature minimum region were determined from Fe I $5435{\AA}$ line data taken by the Fast Imaging Solar Spectrograph (FISS) of the 1.6 m Goode solar Telescope (GST) at the Big Bear Solar Observatory. As a result, we discovered 4 events of oscillations which appear to be internally excited. We analyze their characteristics and relation to photospheric features. Based on these results, we estimate the contribution of the internal excitation for umbral oscillations and discuss their importance.

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Velocity oscillations in the Chromosphere above a Solar Quiet Region

  • Kwak, Hannah;Chae, Jongchul
    • The Bulletin of The Korean Astronomical Society
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    • v.43 no.2
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    • pp.58.3-59
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    • 2018
  • We investigate velocity oscillations in a solar quiet region by using the spectral data of the $H{\alpha}$ and Ca II $8542{\AA}$ lines. The data were acquired by the Fast Imaging Solar Spectrograph installed at the 1.6 m Goode Solar Telescope of Big Bear Solar Observatory. According to Chae & Litvinenko (2018)'s theoretical work, there is a correlation between dominant period of the oscillations and the temperature of the temperature minimum region in a non-isothermal atmosphere. In our study, we measure the temporal variations of the intensity and the line of sight Doppler velocity, and find out the relations between the intensity and dominant period of the oscillations. In addition, we investigate oscillations in a few distinct regions and discuss regional characteristics of the oscillations.

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Tiny Pores Observed by New Solar Telescope and Hinode

  • Cho, Kyung-Suk;Bong, Su-Chan;Chae, Jong-Chul;Kim, Yeon-Han;Park, Young-Deuk;Ahn, K.;Katsukawa, Y.
    • The Bulletin of The Korean Astronomical Society
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    • v.36 no.1
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    • pp.37.2-37.2
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    • 2011
  • Our previous study on tiny pores (R < 2") observed by HINODE/Solar Optical Telescope (SOT) revealed that the plasma in the pores at the photosphere is always moving down and the pores are surrounded by the strong downward motions (highly red-shifted) of neighboring granulations. From this study, we speculated that the flow motions above the pore should be related with the motions at the photosphere, since the pore is strong magnetic field region. Meanwhile, SNU and KASI installed Fast Imaging Solar Spectrograph (FISS) in the Cude room of the 1.6 m New Solar Telescope (NST) at Big Bear Solar Observatory. FISS is a unique system that can do imaging of H-alpha and Ca II 8542 band simultaneously, which is quite suitable for studying of dynamics of chromosphere. To get some clue on the relationship between the photospheric and low-chromospheric motions at the pore region, we took a coordinate observation with NST/FISS and Hinode/SOT for new emerging active region (AR11117) on October 26, 2010. In the observed region, we could find two tiny pores and two small magnetic islands (SMIs), which have similar magnetic flux with the pores but does not look dark. Magnetic flux density and Doppler velocities at the photosphere are estimated by applying the center-of-gravity (COG) method to the HINODE/spectropolarimeter (SP) data. The line-of-sight motions above the photosphere are determined by adopting the bisector method to the wing spectra of Ha and CaII 8542 lines. As results, we found the followings. (1) There are upflow motion on the pores and downflow motion on the SMIs. (2) Towards the CaII 8542 line center, upflow motion decrease and turn to downward motion in pores, while the speed of down flow motion increases in the SMIs. (3) There is oscillating motion above pores and the SMIs, and this motion keep its pattern along the height. (4) As height increase, there is a general tendency of the speed shift to downward on pores and the SMIs. This is more clearly seen on the other regions of stronger magnetic field. In this talk, we will present preliminary understanding of the coupling of pore dynamics between the photosphere and the low-chromosphere.

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OBSERVATION SYSTEM OF SOLAR FLARE TELESCOPE (태양플레어망원경의 관측 시스템)

  • Park, Young-Deuk;Moon, Yong-Jae;Jang, Be-Ho;Sim, Kyung-Jin
    • Publications of The Korean Astronomical Society
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    • v.12 no.1
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    • pp.35-45
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    • 1997
  • SOFT($\underline{So}lar\;\underline{F}lare\;\underline{T}elescope$) installed at BOAO(Bohyunsan Optical Astronomy Observatory) is purposed for observing solar active regions using four refractors on single mount with a $400"\times300"$ field of view: Two refractors with a diameter of 15cm(f15) are observe the white light and $H\alpha$, and the other two refractors with a diameter of 20cm(f8) are observe the magnetic field distribution and Doppler shifts at the solar chromosphere. Three Lyot filters, one of the most important observational instruments, are installed on the optical rails for VMG, LMG, and $H\alpha$ that possible to very narrow pass band observation under high precision stability of temperature. From the combination of KD*P and quarter wave plate in the Lyot filter possible observe the magnetic fields strength and doppler shifts by using the characteristics of polarization components. In this paper, we introduce the basic characteristics, optical system, and monitor system of the SOFT.

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Physics of Solar Flares

  • Magara, Tetsuya
    • The Bulletin of The Korean Astronomical Society
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    • v.35 no.1
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    • pp.26.1-26.1
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    • 2010
  • In this talk we outline the current understanding of solar flares, mainly focusing on magnetohydrodynamic (MHD) processes. A flare causes plasma heating, mass ejection, and particle acceleration which generates high-energy particles. The key physical processes producing a flare are: the emergence of magnetic field from the solar interior to the solar atmosphere (flux emergence), formation of current-concentrated areas (current sheets) in the corona, and magnetic reconnection proceeding in a current sheet to cause shock heating, mass ejection, and particle acceleration. A flare starts with the dissipation of electric currents in the corona, followed by various dynamic processes that affect lower atmosphere such as the chromosphere and photosphere. In order to understand the physical mechanism for producing a flare, theoretical modeling has been develops, where numerical simulation is a strong tool in that it can reproduce the time-dependent, nonlinear evolution of a flare. In this talk we review various models of a flare proposed so far, explaining key features of individual models. We introduce the general properties of flares by referring observational results, then discuss the processes of energy build-up, release, and transport, all of which are responsible for a flare. We will come to a concluding viewpoint that flares are the manifestation of the recovering and ejecting processes of a global magnetic flux tube in the solar atmosphere, which has been disrupted via interaction with convective plasma while rising through the convection zone.

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The Sun Observed by Fast Imaging Solar Spectrograph of the 1.6 meter New Solar Telescope at Big Bear

  • Chae, Jong-Chul;Park, Hyung-Min;Ahn, Kwang-Su;Yang, Hee-Su;Park, Young-Deuk;Nah, Ja-Kyoung;Jang, Bi-Ho;Cho, Kyung-Suk;Cao, Wenda;Gorceix, Nicholas;Goode, Philip R.
    • The Bulletin of The Korean Astronomical Society
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    • v.35 no.2
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    • pp.25-25
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    • 2010
  • With the aim of resolving important physical problems in the chromosphere of the Sun, we developed the Fast Imaging Solar Spectrograph for several years, and at last successfully installed it in the Coude room of the 1.6 meter New Solar Telescope at Big Bear in 2010 May. The instrument is an Echelle spectrograph with imaging capability based on slit scan, and can record two spectral bands (e.g., H alpha band and Ca II 8542 band) simultaneously. The early runs of the instrument produced data of high quality that are suited for the study of quiet Sun, filaments on the disk, prominences outside the limb, active regions and sunspots. We are ready to do good solar sciences using our own instrument, and will be able to do best sciences with the coming improvement of spatial resolution.

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