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  • 1
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    Splay fault slip during the Mw 8.8 2010 Maule Chile earthquake: REPLY (2013)
    Geological Society of America (GSA)
    In: Geology
    Details
    Publication Date: 2013-11-22
    Print ISSN: 0091-7613
    Electronic ISSN: 1943-2682
    Topics: Geosciences
    Published by Geological Society of America (GSA)
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  • 2
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    Grouted sediment slices show signs of earthquake shaking (2001)
    In:  Eos Trans. AGU, Minsk, Elsevier Scientific Publishing Company, vol. 82, no. 49, pp. 603, pp. B12308
    Details
    Publication Date: 2001
    Keywords: paleo ; Seismology ; Geol. aspects ; 7221 ; Seismology ; Paleoseismology ; 1829 ; Hydrology ; Groundwater ; hydrology ; 7294 ; Instruments ; and ; techniques
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    BIBLIOGRAPHY SEISMOLOGY
  • 3
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    Tsunami geology and its role in hazard mitigation (2005)
    In:  Eos Trans. AGU, Minsk, Elsevier Scientific Publishing Company, vol. 86, no. 42, pp. 400, pp. B12308
    Details
    Publication Date: 2005
    Description: The timely topic of tsunami geology was addressed during a recent international workshop sponsored by the U.S. National Science Foundation (NSF). Participants from 15 nations compared criteria for identifying tsunamis by their geologic signatures; explored applications to plate tectonics, hazard assessment, and public education; and discussed recommendations for research priorities. A post-workshop trip occasioned heartfelt exchanges with Washington state coastal residents two days after a local tsunami scare. The workshop was prompted by the Indian Ocean tsunami of 26 December 2004, and began with several presentations about that tsunami and about the lessons being learned from it. Lacking documented precedent in its source region, the 2004 catastrophe provided a horrific reminder of a practical problem: Written and instrumental records rarely span enough time to warn of the full range of a region's tsunami hazards
    Keywords: Earthquake hazard ; Tsunami(s) ; Geol. aspects ; outreach ; paleo ; Seismology ; Proceedings of a conference ; 4564 ; Oceanography: ; Physical: ; Tsunamis ; and ; storm ; surges ; 7221 ; Seismology: ; Paleoseismology ; 4217 ; Oceanography: ; General: ; Coastal ; processes
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    BIBLIOGRAPHY SEISMOLOGY
  • 4
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    Source of the 1730 Chilean earthquake from historical records: implications for the future tsunami hazard on the coast of Metropolitan Chile (2017)
    Wiley
    Details
    Publication Date: 2017-05-02
    Description: Historical records of an earthquake that occurred in 1730 affecting Metropolitan Chile provide essential clues on the source characteristics for the future earthquakes in the region. The earthquake and tsunami of 1730 have been recognized as the largest to occur in Metropolitan Chile since the beginning of written history. The earthquake destroyed buildings along 〉1000 km of the coast and produced a large tsunami that caused damage as far as Japan. Here, its source characteristics are inferred by comparing local tsunami inundations computed from hypothetical earthquakes with varying magnitude and depth, with those inferred from historical observations. It is found that a 600-800 km long rupture involving average slip amounts of 10-14 m (Mw 9.1-9.3) best explains the observed tsunami heights and inundations. This large earthquake magnitude is supported by the 1730 tsunami heights inferred in Japan. The inundation results combined with local uplift reports suggest a southward increase of the slip depth along the rupture zone of the 1730 earthquake. While shallow slip on the area to the north of the 2010 earthquake rupture zone is required to explain the reported inundation, only deeper slip at this area can explain the coastal uplift reports. Since the later earthquakes of the region involved little or no slip at shallow depths, the near future earthquakes on Metropolitan Chile could release the shallow slip accumulated since 1730 and thus lead to strong tsunami excitation. Moderate shaking from a shallow earthquake could delay tsunami evacuation for the most populated coastal region of Chile. (250/250)
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 5
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    Reexamination of the magnitudes for the 1906 and 1922 Chilean earthquakes using Japanese tsunami amplitudes: implications for source depth constraints (2016)
    Wiley
    Details
    Publication Date: 2016-12-15
    Description: Far-field tsunami records from the Japanese tide gauge network allow the reexamination of the moment magnitudes (Mw) for the 1906 and 1922 Chilean earthquakes, which to date rely on limited information mainly from seismological observations alone. Tide gauges along the Japanese coast provide extensive records of tsunamis triggered by six great (Mw 〉8) Chilean earthquakes with instrumentally-determined moment magnitudes. These tsunami records are used to explore the dependence of tsunami amplitudes in Japan on the parent earthquake magnitude of Chilean origin. Using the resulting regression parameters together with tide gauge amplitudes measured in Japan we estimate apparent moment magnitudes of Mw 8.0-8.2 and Mw 8.5-8.6 for the 1906 central and 1922 north-central Chile earthquakes. The large discrepancy of the 1906 magnitude estimated from the tsunami observed in Japan as compared with those previously determined from seismic waves (Ms 8.4), suggests a deeper than average source with reduced tsunami excitation. A deep dislocation along the Chilean megathrust would favor uplift of the coast rather than beneath the sea, giving rise to a smaller tsunami, and producing effects consistent with those observed in 1906. The 1922 magnitude inferred from far-field tsunami amplitudes appear to better explain the large extent of damage and the destructive tsunami that were locally observed following the earthquake than the lower seismic magnitudes (Ms 8.3) that were likely affected by the well-known saturation effects. Thus, a repeat of the large 1922 earthquake poses seismic and tsunami hazard in a region identified as a mature seismic gap
    Print ISSN: 0148-0227
    Topics: Geosciences , Physics
    Published by Wiley on behalf of American Geophysical Union (AGU).
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  • 6
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    H{alpha} kinematics of S4G spiral galaxies - II. Data description and non-circular motions (2015)
    Oxford University Press
    Details
    Publication Date: 2015-06-05
    Description: We present a kinematical study of 29 spiral galaxies included in the Spitzer Survey of Stellar Structure in Galaxies, using Hα Fabry–Perot (FP) data obtained with the Galaxy Hα Fabry–Perot System instrument at the William Herschel Telescope in La Palma, complemented with images in the R band and in Hα. The primary goal is to study the evolution and properties of the main structural components of galaxies through the kinematical analysis of the FP data, complemented with studies of morphology, star formation and mass distribution. In this paper we describe how the FP data have been obtained, processed and analysed. We present the resulting moment maps, rotation curves, velocity model maps and residual maps. Images are available in fits format through the NASA/IPAC Extragalactic Database and the Centre de Données Stellaires. With these data products we study the non-circular motions, in particular those found along the bars and spiral arms. The data indicate that the amplitude of the non-circular motions created by the bar does not correlate with the bar strength indicators. The amplitude of those non-circular motions in the spiral arms does not correlate with either arm class or star formation rate along the spiral arms. This implies that the presence and the magnitude of the streaming motions in the arms is a local phenomenon.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 7
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    Triggered star formation in a merging, gas-rich dwarf galaxy around NGC 7241 (2015)
    Oxford University Press
    Details
    Publication Date: 2015-05-08
    Description: Using multiwavelength kinematic and photometric data we have analysed the gaseous and stellar properties of a previously uncharacterized low-mass star-forming companion and newly discovered stellar stream seen projected against the edge-on spiral galaxy NGC 7241. The companion object was identified serendipitously as an offset velocity component in H α Fabry–Perot observations along the line of sight to NGC 7241, and is most prominent visually in UV and blue wavelengths. Its occulting position with respect to NGC 7241 allows measurement of its dust extinction properties which are then combined with photometric spectral energy distribution fitting and long-slit spectroscopy to study star formation (SF) in this gas-rich accreting dwarf galaxy. The dynamical properties of the stream and companion suggest that they may likely be remnants of the same low-mass progenitor dwarf galaxy which is being disrupted during its accretion on to NGC 7241 – with the companion's recent SF triggered during its passage with the disc of NGC 7241. This is supported by the companion's metallicity and SF rates, the asymmetric SF in the disc of NGC 7241, as well as the coincident velocity of the extraplanar H i filament and the star-forming companion. In contrast, mass estimates from dynamical modelling of NGC 7241 rule out an interaction between NGC 7241 and UGC 11964 (the other large spiral galaxy in the group) within the last ~3 Gyr – making such an interaction a poor candidate for inducing the recent SF in the system. Together, the data for this system offer a window into how SF proceeds in low-mass mergers.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 8
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    Comparative internal kinematics of the H II regions in interacting and isolated galaxies: implications for massive star formation modes (2015)
    Oxford University Press
    Details
    Publication Date: 2015-06-07
    Description: We have observed 12 interacting galaxy pairs using the Fabry–Perot interferometer GH αFaS (Galaxy H α Fabry–Perot system) on the 4.2-m William Herschel Telescope at the Observatorio del Roque de los Muchachos, La Palma. We present here the Hα surface brightness, velocity and velocity dispersion maps for the 10 systems we have not previously observed using this technique, as well as the physical properties (sizes, Hα luminosities and velocity dispersion) of 1259 H ii regions from the full sample. We also derive the physical properties of 1054 H ii regions in a sample of 28 isolated galaxies observed with the same instrument in order to compare the two populations of H ii regions. We find a population of the brightest H ii regions for which the scaling relations, for example the relation between the Hα luminosity and the radius, are clearly distinct from the relations for the regions of lower luminosity. The regions in this bright population are more frequent in the interacting galaxies. We find that the turbulence, and also the star formation rate (SFR), are enhanced in the H ii regions in the interacting galaxies. We have also extracted the Hα equivalent widths for the H ii regions of both samples, and we have found that the distribution of H ii region ages coincides for the two samples of galaxies. We suggest that the SFR enhancement is brought about by gas flows induced by the interactions, which give rise to gravitationally bound gas clouds which grow further by accretion from the flowing gas, producing conditions favourable to star formation.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 9
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    Comparative internal kinematics of the H II regions in interacting and isolated galaxies: implications for massive star formation modes (2015)
    Oxford University Press
    Details
    Publication Date: 2015-06-12
    Description: We have observed 12 interacting galaxy pairs using the Fabry–Perot interferometer GH αFaS (Galaxy H α Fabry–Perot system) on the 4.2-m William Herschel Telescope at the Observatorio del Roque de los Muchachos, La Palma. We present here the Hα surface brightness, velocity and velocity dispersion maps for the 10 systems we have not previously observed using this technique, as well as the physical properties (sizes, Hα luminosities and velocity dispersion) of 1259 H ii regions from the full sample. We also derive the physical properties of 1054 H ii regions in a sample of 28 isolated galaxies observed with the same instrument in order to compare the two populations of H ii regions. We find a population of the brightest H ii regions for which the scaling relations, for example the relation between the Hα luminosity and the radius, are clearly distinct from the relations for the regions of lower luminosity. The regions in this bright population are more frequent in the interacting galaxies. We find that the turbulence, and also the star formation rate (SFR), are enhanced in the H ii regions in the interacting galaxies. We have also extracted the Hα equivalent widths for the H ii regions of both samples, and we have found that the distribution of H ii region ages coincides for the two samples of galaxies. We suggest that the SFR enhancement is brought about by gas flows induced by the interactions, which give rise to gravitationally bound gas clouds which grow further by accretion from the flowing gas, producing conditions favourable to star formation.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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  • 10
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    Interacting galaxies in the nearby Universe: only moderate increase of star formation (2015)
    Oxford University Press
    Details
    Publication Date: 2015-10-09
    Description: We investigate the influence of interactions on the star formation by studying a sample of almost 1500 of the nearest galaxies, all within a distance of ~45 Mpc. We define the massive star formation rate (SFR), as measured from far-IR emission, and the specific star formation rate (SSFR), which is the former quantity normalized by the stellar mass of the galaxy, and explore their distribution with morphological type and with stellar mass. We then calculate the relative enhancement of these quantities for each galaxy by normalizing them by the median SFR and SSFR values of individual control populations of similar non-interacting galaxies. We find that both SFR and SSFR are enhanced in interacting galaxies, and more so as the degree of interaction is higher. The increase is, however, moderate, reaching a maximum of a factor of 1.9 for the highest degree of interaction (mergers). The SFR and SSFR are enhanced statistically in the population, but in most individual interacting galaxies they are not enhanced at all. We discuss how those galaxies with the largest SFR and/or SSFR enhancement can be defined as starbursts. This study is based on a representative sample of nearby galaxies, including many low-mass and dwarf/irregular galaxies, and we argue that it should be used to place constraints on studies based on samples of galaxies at larger distances, beyond the local Universe.
    Print ISSN: 0035-8711
    Electronic ISSN: 1365-2966
    Topics: Physics
    Published by Oxford University Press
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