http://chineseinput.net/에서 pinyin(병음)방식으로 중국어를 변환할 수 있습니다.
변환된 중국어를 복사하여 사용하시면 됩니다.
Kumar, Pankaj,Innes, D. E.,Cho, Kyung-Suk American Astronomical Society 2016 The Astrophysical journal Vol.828 No.1
<P>This paper presents multiwavelength observations of a flare-generated type II radio burst. The kinematics of the shock derived from the type II burst closely match a fast extreme ultraviolet (EUV) wave seen propagating through coronal arcade loops. The EUV wave was closely associated with an impulsive M1.0 flare without a related coronal mass ejection, and was triggered at one of the footpoints of the arcade loops in active region NOAA 12035. It was initially observed in the 335 angstrom images from the Atmospheric Image Assembly with a speed of similar to 800 km s(-1) and it accelerated to similar to 1490 km s(-1) after passing through the arcade loops. A fan-spine magnetic topology was revealed at the flare site. A small, confined filament eruption (similar to 340 km s(-1)) was also observed moving in the opposite direction to the EUV wave. We suggest that breakout reconnection in the fan-spine topology triggered the flare and associated EUV wave that propagated as a fast shock through the arcade loops.</P>
THE SOURCE REGIONS OF SOLAR ENERGETIC PARTICLES DETECTED BY WIDELY SEPARATED SPACECRAFT
Park, Jinhye,Innes, D. E.,Bucik, R.,Moon, Y.-J. IOP Publishing 2013 The Astrophysical journal Vol.779 No.2
<P>We studied the source regions of 12 solar energetic particle (SEP) events seen between 2010 August and 2012 January at STEREO-A, B, and/or Earth (Advanced Composition Explorer/Solar and Heliospheric Observatory/GOES), when the two STEREO spacecraft were separated by about 180 degrees. All events were associated with flares (C1 to X6) and fast coronal mass ejections and, except for one, accompanied by type II radio bursts. We have determined the arrival times of the SEPs at the three positions. Extreme ultraviolet (EUV) waves, observed in the 195 angstrom and 193 angstrom channels of STEREO and the Solar Dynamics Observatory, are tracked across the Sun to determine their arrival time at the photospheric source of open field lines connecting to the spacecraft. There is a good correlation between the EUV wave arrival times at the connecting footpoints and the SEP onset times. The delay time between electron onset and the EUV wave reaching the connecting footpoint is independent of distance from the flare site. The proton delay time increases with distance from the flare site. In three of the events, secondary flare sites may have also contributed to the wide longitudinal spread of SEPs.</P>
PARTIAL REFLECTION AND TRAPPING OF A FAST-MODE WAVE IN SOLAR CORONAL ARCADE LOOPS
Kumar, Pankaj,Innes, D. E. IOP Publishing 2015 ASTROPHYSICAL JOURNAL LETTERS - Vol.803 No.2
<P>We report on the first direct observation of a fast-mode wave propagating along and perpendicular to cool (171 angstrom) arcade loops observed by the Solar Dynamics Observatory/Atmospheric Imaging Assembly (AIA). The wave was associated with an impulsive/compact flare near the edge of a sunspot. The EUV wavefront expanded radially outward from the flare center and decelerated in the corona from 1060 to 760 km s(-1) within similar to 3-4 minutes. Part of the EUV wave propagated along a large-scale arcade of cool loops and was partially reflected back to the flare site. The phase speed of the wave was about 1450 km s(-1), which is interpreted as a fast-mode wave. A second overlying loop arcade, orientated perpendicular to the cool arcade, is heated and becomes visible in the AIA hot channels. These hot loops sway in time with the EUV wave, as it propagated to and fro along the lower loop arcade. We suggest that an impulsive energy release at one of the footpoints of the arcade loops causes the onset of an EUV shock wave that propagates along and perpendicular to the magnetic field.</P>
Talandis,Jonas,Innes,J,D,Cox,A,W 한국화재소방학회 1997 한국화재소방학회 학술대회 논문집 Vol.1997 No.-
The cone calorimeter as defined by ISO 5660, ASTM 1354, and NFPA 264A is used to assess the reaction to fire of almost any material that must be evaluated in the fire science field. Typical combustion gas analyses include oxygen, CO and CO2. Oxygen consumption is used to determine rate of heat release. Analysis of combustion gases other than oxygen, CO and CO2 has been attempted using filters to remove the solid smoke particles before analysis. This method has generated unreliable results due to the adsorption of many gas components on the active carbon . particles deposited on the filters. A technique using fourier Transform Infrared (FTIB) analysis without filtration will be disclosed and a discussion will be presented of the analytical results of toxic gases produced from various flame retarded polymeric materials. Use of such data in lethal toxic potency determinations is also reviewed.
UNDERCOVER EUV SOLAR JETS OBSERVED BY THE INTERFACE REGION IMAGING SPECTROGRAPH
Chen, N.-H.,Innes, D. E. American Astronomical Society 2016 The Astrophysical journal Vol.833 No.1
<P>It is well-known that extreme ultraviolet (EUV) emission emitted at the solar surface is absorbed by overlying cool plasma. Especially in active regions, dark lanes in EUV images suggest that much of the surface activity is obscured. Simultaneous observations from the Interface Region Imaging Spectrograph, consisting of UV spectra and slit-jaw images (SJI), give vital information with sub-arcsecond spatial resolution on the dynamics of jets not seen in EUV images. We studied a series of small jets from recently formed bipole pairs beside the trailing spot of active region 11991, which occurred on 2014 March 5 from 15: 02: 21 UT to 17: 04: 07 UT. Collimated outflows with bright roots were present. in. SJI 1400 angstrom (transition region) and 2796 angstrom (upper chromosphere) that were mostly not seen in Atmospheric Imaging Assembly (AIA) 304 angstrom (transition region) and AIA 171 angstrom (lower corona) images. The Si IV spectra show a. strong blue. wing enhancement, but no red. wing, in the line profiles of the ejecta for all recurrent jets, indicating outward flows without twists. We see two types of Mg II line profiles produced by the jets spires: reversed and non-reversed. Mg II lines remain optically thick, but turn. optically thin in the highly Doppler shifted wings. The energy flux contained in each recurrent jet is estimated using a velocity differential emission measure technique that. measures the emitting power of the plasma as a function of the line-of-sight velocity. We found that all the recurrent jets release similar energy (10(8) erg cm(-2) s(-1)) toward the corona and the downward component is less than 3%.</P>