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Official Journal of the Asia Oceania Geosciences Society (AOGS)

Table 2 Summarizing table

From: Infrasound and seismic detections associated with the 7 September 2015 Bangkok fireball

Station Calculated range (Km) Calculated back azimuth (\(^{\circ }\)) Calculated arrival time UTC (c = 340 m/s) Observed arrival time (UTC) from PMCC Observed back azimuth (\(^{\circ }\)) from PMCC Trace velocity (m/s) from PMCC Celerity (m/s) Max amplitude of the beam from Inferno (in dB) Period at max amplitude from Inferno (beam, in s) Range for period of max amplitude from Inferno (beam, in s) Total energy (kt) Error on total energy estimate (kt) Stratospheric wind speed (m/s)
SING 1558 335 03:03:02 03:07:13 337.9 365 322 64.85 5.01 5.3088–4.7315 1.15 ±0.24 0.93
I06AU 2910 2 04:09:16 04:27:08 3.0 348 298 61.27 3.16 3.3497–2.9854 0.25 ±0.05 3.07
I04AU 5738 337 06:27:56 07:06:41 335.7 352 299 69.70 4.47 4.7315–4.2170 0.78 ±0.17 10.13
I53US 9703 298 09:42:17 10:40:19 297.4 345 303 39.23 4.47 4.7315–4.2170 0.78 ±0.17 3.43
  1. Table summarizing the calculated results for this study for each available infrasound station. The range, back azimuths and arrival times are calculated using the JPL origin time and location (Fig. 1). The trace velocity is calculated using the PMCC results and is the velocity of the signal across the array. The celerity is derived from the arrival time determined using PMCC and the origin time (Fig. 2). The Inferno algorithm, which provides high-resolution multispectral analysis in logarithmic frequency space with time-window auto-scaling, was finally used (Garces 2013) to calculate the maximum amplitude and amplitude period bin from the beam for each station. The period is derived from the center frequency of the bin (Fig. 2). The program was set to 6th octave bands. Our observed arrival times are calculated from the PMCC results and represent the arrival of a coherent signal at the station