Old Stellar Populations in Nearby Dwarf Galaxies

What can we learn from the somewhat arduous study of old stellar populations in nearby galaxies? Unless the nearby universe is subtly anomalous, it should contain a relatively normal selection of galaxies whose histories are representative of field galaxies in general throughout the Universe. We can therefore take advantage of our ability to resolve local galaxies into individual stars to directly, and accurately, measure star formation histories. The star formation histories are determined from numerical models, based on stellar evolution tracks, of colour-magnitude diagrams. The most accurate information on star formation rates extending back to the earliest epoches can be obtained from the structure of the main sequence. However, the oldest main sequence turnoffs are very faint, and it is often necessary to use the brighter, more evolved, populations to infer the star formation history at older times. A complete star formation history can be compared with the spectroscopic properties of galaxies seen over a large range of lookback times in redshift surveys. There is considerable evidence that the faint blue galaxies seen in large numbers in cosmological surveys are the progenitors of the late-type irregular galaxies seen in copious numbers in the Local Group, and beyond. We consider how the `Madau-diagram', the star formation history of the Universe, would look if the Local Group were to be considered representative of the Universe as a whole.     

Dwarf galaxies: Important clues to galaxy formation

The smallest dwarf galaxies are the most straight forward objects in which to study star formation processes on a galactic scale. They are typically single cell star forming entities, and as small potentials in orbit around a much larger one they are unlikely to accrete much (if any) extraneous matter during their lifetime (either intergalactic gas, or galaxies) because they will typically lose the competition with the much larger galaxy. We can utilise observations of stars of a range of ages to measure star formation and enrichment histories back to the earliest epochs. The most ancient objects we have ever observed in the Universe are stars found in and around our Galaxy. Their proximity allows us to extract from their properties detailed information about the time in the early Universe into which they were born. A currently fashionable conjecture is that the earliest star formation in the Universe occurred in the smallest dwarf galaxy sized objects. Here I will review some recent observational highlights in the study of dwarf galaxies in the Local Group and the implications for understanding galaxy formation and evolution. This revised version was published online in August 2006 with corrections to the Cover Date.     

Generation of Long Internal Gravity Waves in Waveguides by Rising Buoyant Air Masses and Other Sources

Summary The displacement fields generated in an internal gravity wave waveguide between plane rigid walls are compared for two types of source: an explosive point source and a rising buoyant sphere moving at constant speed. It is concluded that for large enough spheres and comparable energy expenditures, the buoyant sphere is a far more efficient source of long internal gravity waves. In particular it appears possible to conclude that, in the case of large events such as nuclear or volcanic explosions in the atmosphere, the rising heated air mass can generate long wavelength (Λ > 500 km) internal gravity waves at ionospheric heights.     

Hydroacoustic contributions to understanding the December 26th 2004 great Sumatra–Andaman Earthquake

Within the era of modern digital-recording, the December 26th 2004 Sumatra–Andaman Earthquake represents an event of unprecedented scale. Hydroacoustic observations have made significant contributions toward our understanding of this great rupture and serve to reiterate the potential use of tertiary (T) waves as a tool in tsunami warning. Small-aperture arrays of hydrophones operated by the International Monitoring System (IMS) recorded the seismically generated, water-borne T-wave within the Indian Ocean. Due to the velocity structure of the oceanic water column, T-wave propagation is both slower and more efficient than radiation within the solid earth. This results in a relatively large amplitude signal that arrives within a time window distinct from the more complex and overlapping pattern of solid earth seismic phases. Hydroacoustic analysis has constrained the rupture length of the fault to be ~1,200 km and the duration on the order of 8 min, with 2–3 phases exhibiting progressively decreasing rupture velocity. These data also indicate that aftershock rates in the first hours following the mainshock correlate with spatial variability in the sourced T-wave amplitude, with far fewer events along the northern section of the main rupture. Although IMS stations telemeter data in near real time, data access for scientists was restricted due to the provisions of the Comprehensive Test Ban Treaty. The swift dissemination of data will be critical in using hydroacoustic methods to assess the magnitude and tsunamigenic potential of future events.     

Aftershock sequences in the mid-ocean ridge environment: an analysis using hydroacoustic data

Hydroacoustic data from autonomous arrays and the U.S. Navy's Sound Surveillance System (SOSUS) provide an opportunity to examine the temporal and spatial properties of seismicity along portions of the slow-spreading Mid-Atlantic Ridge (MAR), intermediate-spreading Juan de Fuca Ridge (JdFR) and fast-spreading East Pacific Rise (EPR). Aftershock and foreshock events are selected from the hydroacoustic earthquake catalog using single-link cluster (SLC) analysis, with a combined space–time metric. In the regions examined, hydroacoustic data improve the completeness level of the earthquake catalog by 1.5–2.0 orders of magnitude, allowing the decay constant, p, of the modified Omori law (MOL) to be determined for individual sequences. A non-parametric goodness-of-fit test indicates six of the seven sequences examined are described well by a MOL model. The p-values obtained for individual ridge and transform sequences using hydroacoustic data are larger than that previously estimated from the analysis of a stacked sequence generated from teleseismic data. For three sequences along the Siqueiros, Discovery and western Blanco Transforms, p-values are estimated to be 0.94–1.29. The spatial distribution of aftershocks suggests that the mainshock rupture is constrained by intra-transform spreading centers at these locations. An aftershock sequence following a 7.1M_s thrust event near the northern edge of the Easter Microplate exhibits p=1.02±0.11. Within the sequence, aftershocks are located to the north of a large topographic ridge, which may represent the surface expression of the shallow-dipping fault that ruptured during the mainshock. Two aftershock sequences near 24°25′N and 16°35′N on the MAR exhibit higher p-values, 1.74±0.23 and 2.37±1.65, although the latter estimate is not well constrained because of the small number of aftershocks. Larger p-values along the ridge crest might reflect a hotter thermal regime in this setting. Additional monitoring, however, will be needed to determine if p-value differences between the ridge and transform sequences are robust. A 1999 sequence on the Endeavour segment of the JdFR, which has been correlated with changes in the hydrothermal system, is described poorly by the MOL model. The failure of the MOL model, the anomalously large number of earthquakes within the sequence and absence of a clearly dominant mainshock are inconsistent with aftershock activity and the simple tectonic origin that has been proposed previously for this sequence.     

东太平洋海隆轴向热液流动的地震识别

洋中脊轴上的热液循环影响岩石层及上覆海水的化学性质,供养着化合生物群,也是岩石层向海水传递热量的媒介(Slater et al,1980;Stein and Stein,1994;Elderfield and Schultz,1996)。通常认为这个系统中的热液流起源于洋中脊扩张轴处,并由一些离扩张轴较远的断层补给(Lowelletal,1995;Kelley et al,2002;Fisher,2003),但热液系统的结构和规模通常不能直接观察到,而是通过由地球物理条件约束的热模型和地球化学模型推断得到的(Johnson et al,1993;Dunn et al,2000;Lowell and Yao,2002)。使用发生的微震也许能通过揭示热裂缝区说明热液的流动路径,在这些裂缝区域冷水从地壳热岩石中获得热量,另外,一些由岩浆及构造应力作用造成的裂隙增大了这些区域的孔隙度和渗透性。本文指出,东太平洋海隆上得到很好研究的热液喷口场之下的震源群集于一小尺度轴向不连续面附近的垂向管状区域和轴向岩浆房正上方的带内。该浅层管状群集相对于这一段洋脊上热液喷口的分布和温度的位置表明,热液补充量集中在那里是构造破裂引起渗...