A New Catalog of Explosion Source Parameters in the Utah Region with Application to ML–MC‐Based Depth Discrimination at Local Distances

2019 ◽  
Vol 91 (1) ◽  
pp. 222-236 ◽  
Author(s):  
Jonathan R. Voyles ◽  
Monique M. Holt ◽  
J. Mark Hale ◽  
Keith D. Koper ◽  
Relu Burlacu ◽  
...  

Abstract A catalog of explosion source parameters is valuable for testing methods of source classification in seismically active regions. We develop a manually reviewed catalog of explosions in the Utah region for 1 October 2012 to 30 June 2018 and use it to assess a newly proposed, magnitude‐based depth discriminant. Within the Utah region we define 26 event clusters that are primarily associated with mine blasts but also include explosions from weapons testing and disposal. The catalog refinement process consists of confirming the explosion source labels, revising the local (ML) and coda duration (MC) magnitudes, and relocating the hypocenters. The primary features used to determine source labels are waveform characteristics such as frequency content, the proximity of the preliminary epicenter to a permitted blast region, the time of day, and prior notification from mine operators. We reviewed 2199 seismic events of which 1545 are explosions, 459 are local earthquakes, and 195 are other event types. Of the reviewed events, 127 (5.8%) were reclassified with new labels. Over 74% of the reviewed explosions have both ML and MC, a sizable improvement over the unreviewed catalog (65%). The mean ML–MC value for the new explosion catalog is −0.196±0.017 (95% confidence interval) compared with a previously determined value of 0.048±0.008 for naturally occurring earthquakes in the Utah region. The shallow depths of the explosions lead to enhanced coda production, which in turn leads to anomalously large MC values. This finding confirms that ML–MC is a useful metric for discriminating explosions from deeper tectonic earthquakes in Utah. However, there is significant variation in ML–MC among the 26 explosion source regions, suggesting that ML–MC observations should be combined with other classification metrics to achieve the best performance in distinguishing explosions from earthquakes.

2013 ◽  
Vol 8 (S300) ◽  
pp. 209-214 ◽  
Author(s):  
Lucie M. Green ◽  
Bernhard Kliem

AbstractUnderstanding the magnetic configuration of the source regions of coronal mass ejections (CMEs) is vital in order to determine the trigger and driver of these events. Observations of four CME productive active regions are presented here, which indicate that the pre-eruption magnetic configuration is that of a magnetic flux rope. The flux ropes are formed in the solar atmosphere by the process known as flux cancellation and are stable for several hours before the eruption. The observations also indicate that the magnetic structure that erupts is not the entire flux rope as initially formed, raising the question of whether the flux rope is able to undergo a partial eruption or whether it undergoes a transition in specific flux rope configuration shortly before the CME.


2019 ◽  
Vol 486 (4) ◽  
pp. 4936-4946 ◽  
Author(s):  
P Vemareddy

Abstract Using time-sequence vector magnetic field observation from Helioseismic and Magnetic Imager, we examined the connection of non-neutralized currents and the observed activity in 20 solar active regions (ARs). The net current in a given magnetic polarity is algebraic sum of direct current (DC) and return current (RC) and the ratio |DC/RC| is a measure of degree of net current neutralization (NCN). In the emerging ARs, the non-neutrality of these currents builds with the onset of flux emergence, following the relaxation to neutrality during the separation motion of bipolar regions. Accordingly, some emerging ARs are source regions of CMEs occurring at the time of higher level non-neutrality. ARs in the post-emergence phase can be CME productive provided they have interacting bipolar regions with converging and shearing motions. In these cases, the net current evolves with higher level (>1.3) of non-neutrality. Differently, the |DC/RC| in flaring and quiet ARs vary near unity. In all the AR samples, the |DC/RC| is higher for chiral current density than that for vertical current density. Owing to the fact that the non-neutralized currents arise in the vicinity of sheared polarity-inversion-lines (SPILs), the profiles of the total length of SPIL segments and the degree of NCN follow each other with a positive correlation. We find that the SPIL is localized as small segments in flaring-ARs, whereas it is long continuous in CME-producing ARs. These observations demonstrate the dividing line between the CMEs and flares with the difference being in global or local nature of magnetic shear in the AR that reflected in non-neutralized currents.


2019 ◽  
Vol 2019 ◽  
pp. 1-14 ◽  
Author(s):  
L. Lei ◽  
Q. Zhong ◽  
J. Wang ◽  
L. Shi ◽  
S. Liu

The solar radio flux at 10.7cm (F10.7) is a direct monitor and an important indicator of solar variability, and F10.7 is commonly used in empirical atmospheric models, ionosphere models, etc. The source regions of F10.7 are mainly in the corona above the active regions, and the extreme ultraviolet (EUV) images reflect the coronal thermal structure. In this paper, an index is defined as PSR based on the intensity values of solar EUV images to represent the coronal contribution to F10.7. The Spearman correlation coefficient between the observed values of F10.7 and PSR is 0.85 in 304 Å EUV images. Based on the high correlation, an empirical model is constructed. Combining the EUV data of SDO/AIA and the twin STEREO/EUVI, solar full-disk EUV images can be generated, and the future 27-day values of PSR can be calculated. Then, a realistic estimation of F10.7 from 1 to 27 days in advance can be provided by the empirical model. Compared to the predictive values of F10.7 by the 54th-order autoregressive models in 2012-2013, the error drop-rate of our model is 12.54%, and our method has significant advantages in the upcoming 3 to 27 days’ forecast.


Author(s):  
B. Filippov

Abstract Coronal mass ejections (CMEs) are tightly related to filament eruptions and usually are their continuation in the upper solar corona. It is common practice to divide all observed CMEs into fast and slow ones. Fast CMEs usually follow eruptive events in active regions near big sunspot groups and associated with major solar flares. Slow CMEs are more related to eruptions of quiescent prominences located far from active regions. We analyse 10 eruptive events with particular attention to the events on 2013 September 29 and on 2016 January 26, one of which was associated with a fast CME, while another was followed by a slow CME. We estimated the initial store of free magnetic energy in the two regions and show the resemblance of pre-eruptive situations. The difference of late behaviour of the two eruptive prominences is a consequence of the different structure of magnetic field above the filaments. We estimated this structure on the basis of potential magnetic field calculations. Analysis of other eight events confirmed that all fast CMEs originate in regions with rapidly changing with height value and direction of coronal magnetic field.


Author(s):  
Bei Wang ◽  
Rebecca M. Harrington ◽  
Yajing Liu ◽  
Honn Kao ◽  
Hongyu Yu

ABSTRACT On 17 August 2015, an Mw 4.6 earthquake occurred northwest of Fort St. John, British Columbia, possibly induced by hydraulic fracturing (HF). We use data from eight broadband seismometers located ∼50  km from the hypocenter to detect and estimate source parameters of more than 300 events proximal to the mainshock. Stress-drop values estimated using seismic moment and corner frequency from single-event spectra and spectral ratios range from ∼1 to 35 MPa, within the typical range of tectonic earthquakes. We observe an ∼5-day delay between the onset of fluid injection and the mainshock, a b-value of 0.78 for the sequence, and a maximum earthquake magnitude larger than the prediction based on the total injection volume, suggesting that the Mw 4.6 sequence occurred on a pre-existing fault and that the maximum magnitude is likely controlled by tectonic conditions. Results presented here show that pre-existing fault structures should be taken into consideration to better estimate seismic hazard associated with HF operations and to develop schemes for risk mitigation in close proximity to HF wells.


2019 ◽  
Vol 177 (5) ◽  
pp. 1917-1929 ◽  
Author(s):  
Ken Miyakoshi ◽  
Kazuhiro Somei ◽  
Kunikazu Yoshida ◽  
Susumu Kurahashi ◽  
Kojiro Irikura ◽  
...  

Author(s):  
Stefano Carlino ◽  
Nicola Alessandro Pino ◽  
Anna Tramelli ◽  
Vincenzo De Novellis ◽  
Vincenzo Convertito

AbstractThe island of Ischia, located in the Gulf of Naples, represents an unusual case of resurgent caldera where small-to-moderate magnitude volcano-tectonic earthquakes generate large damage and catastrophic effects, as in the case of 4 March 1881 (Imax-VIII-IXMCS) and 28 July 1883 (Imax X-XI MCS) historical earthquakes, and of the recent 21 August 2017 MW = 3.9, event. All these earthquakes struck the northern area of the island. With about 65,000 inhabitants, Ischia is a popular touristic destination for thermals baths, hosting more than 3,000,000 visitors per year, thus representing a high seismic risk area. Assessing its seismic potential appears a fundamental goal and, to this end, the estimate of the magnitude of significant historical events and the characterization of their source are crucial. We report here a reassessment of historical data of damage of 1881 and 1883 earthquakes to evaluate the main source parameters of these events (obtained with the BOXER and EXISM software) and quantitatively compare, for the first time, the results with the source characteristics, obtained from instrumental data, of the recent 2017 earthquake. The results allowed us to assess the location, as well as the possible dimension and the related maximum magnitude, of the seismogenic structure responsible for such damaging earthquakes. Our results also provide an additional framework to define the mechanisms leading to earthquakes associated with the dynamics of calderas.


2002 ◽  
Vol 82 (3) ◽  
pp. 567-577 ◽  
Author(s):  
R. J. N. Emery ◽  
N. G. Munier-Jolain ◽  
A-S. Voisin ◽  
C. Salon

Xylem-mobile Na+ in peas appears to have the attributes of a convenient marker for estimates of root biomass. This study examined the consistency and predictability of biomass-based, root to shoot Na+ delivery rates. In glasshouse experiments, xylem Na+ delivery was studied according to changing exogenous pressure regimes, time of day of xylem sap extraction, plant development, soil Na+ concentration and xylem sap extraction methods. At a given developmental stage, Na+ delivery in relation to root biomass was constant and independent of xylem water flux. This relationship held providing that collections were made for at least 60 min, the nature of xylem sap extraction (natural root pressure, vacuum or external pressure) was the same and Na+ concentration in the nutrient solution was constant and below 2.5 mM. A negative linear relationship was found between-biomass based Na+ delivery and development (degree days after emergence), with declining values likely caused by overestimates of viable root biomass. Likewise, in the field, Na+ delivery rates occurred predictably with soil Na+, as long as soil Na+ was not increased beyond 5-fold that of naturally occurring levels. Field biomass-based Na+ delivery was largely unaffected by changes in development from early flowering to late seed filling. If used within the defined methodological and developmental limits, Na+ delivery can be a valuable time and labour saving tool for calculating numerous root biomass characteristics, particularly in soil substrates that hamper accurate root recovery. Key words: Controlled conditions, field, Na+ uptake, pea, root biomass, xylem delivery


Solar Physics ◽  
2021 ◽  
Vol 296 (8) ◽  
Author(s):  
David Stansby ◽  
Lucie M. Green ◽  
Lidia van Driel-Gesztelyi ◽  
Timothy S. Horbury

AbstractBoth coronal holes and active regions are source regions of the solar wind. The distribution of these coronal structures across both space and time is well known, but it is unclear how much each source contributes to the solar wind. In this study we use photospheric magnetic field maps observed over the past four solar cycles to estimate what fraction of magnetic open solar flux is rooted in active regions, a proxy for the fraction of all solar wind originating in active regions. We find that the fractional contribution of active regions to the solar wind varies between 30% to 80% at any one time during solar maximum and is negligible at solar minimum, showing a strong correlation with sunspot number. While active regions are typically confined to latitudes ±30∘ in the corona, the solar wind they produce can reach latitudes up to ±60∘. Their fractional contribution to the solar wind also correlates with coronal mass ejection rate, and is highly variable, changing by ±20% on monthly timescales within individual solar maxima. We speculate that these variations could be driven by coronal mass ejections causing reconfigurations of the coronal magnetic field on sub-monthly timescales.


2021 ◽  
Vol 8 ◽  
Author(s):  
José Ángel López-Comino ◽  
Thomas Braun ◽  
Torsten Dahm ◽  
Simone Cesca ◽  
Stefania Danesi

On October 27, 2017, an Mw 4 earthquake occurred close to the municipality of Montesano sulla Marcellana, less than 10 km external to the concession of the largest European onshore hydrocarbon reservoir—the Val d’Agri oilfield (Southern Italy). Being a weak event located outside the extended monitoring domain of the industrial concession, the relevance of this earthquake and the possible links with the hydrocarbon exploitation were not extensively discussed. Actually, the analysis of shallow seismic events close to subsurface exploitation domains plays a significant role in the definition of key parameters in order to discriminate between natural, triggered, and induced seismicity, especially in tectonically active regions. The study of weak-to-moderate earthquakes can improve the characterization of the potentially destructive seismic hazard of this particular area, already struck by M > 6.5 episodes in the past. In this work, we analyze the source parameters of this Mw 4 earthquake by applying advanced seismological techniques to estimate the uncertainties derived from the moment tensor inversion and identify plausible directivity effects. The moment tensor is dominated by a NW–SE oriented normal faulting with a centroid depth of 14 km. A single ML 2.1 aftershock was recorded and used as the empirical Green’s function to calculate the apparent source time function for the mainshock. Apparent durations (in the range 0.11–0.21 s, obtained from S-waves) define an azimuthal pattern, which reveals an asymmetric bilateral rupture with 70% of the rupture propagation in the N310°W direction, suggesting a rupture plane dipping to the SW. Our results tally with the activation of a deeper fault segment associated with the Eastern Agri Fault System close to the basement as the origin of the Montesano earthquake. Finally, the Coulomb stress rate induced by depletion of the oilfield is calculated to quantify the trigger potential estimated for the Montesano earthquake yielding relatively low probabilities below 10%. Our analyses point toward the conclusion that the Mw 4 event was more likely due to the local natural tectonic stress, rather than induced or triggered by the long-term hydrocarbon extraction in the Val d’Agri oilfield.


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