54 research outputs found

    Different roles for prepared and spontaneous thoughts: A practice-based study of musical performance from memory

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    Background in music performance. During musical performance, experienced soloists have a mental map of the music in mind. Landmarks in this map remind them of where they are and what to do next. Background in music psychology. These performance cues (PCs) are prepared during practice so that they come to mind automatically, ensuring that the performance unfolds as planned. Aims. Do musicians use the same PCs in each performance? What other thoughts do they have during performance? Main contribution. To answer these questions, a singer (the first author) reported the thoughts she had as she practised Arnold Schoenberg’s two Songs, Op. 14 (1907-1908), and then again as she performed the songs in a public concert. Seventeen months later, she reconstructed the songs from memory, then performed them and reported her thoughts again. Comparison of the three sets of reports showed that slightly more than half of her thoughts in each of the two performances were PCs, i.e., had occurred during practice, and slightly less than half were spontaneous, new thoughts about the music or performance. The PCs were more stable over time: 17 (25%) occurred in both performances compared to only three (4%) of the spontaneous thoughts. Both PCs and spontaneous thoughts reflected the singer’s current concerns, but in different ways. When the singer performed the songs again after the reconstruction, her thoughts were shaped by the memory problems that she had experienced during the reconstruction that preceded the performance. She thought about the PCs that she had needed to stop at and about the new locations that she had just used as starting places. Implications. PCs are prepared during practice to provide the mental landmarks needed for a secure performance while spontaneous thoughts reflect more transitory experiences and insights

    Lawson Criterion for Ignition Exceeded in an Inertial Fusion Experiment

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    Multi-messenger observations of a binary neutron star merger

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    On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

    The Use of Unusual Psychological Theories in Psychobiography: A Case Study and Discussion

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    This chapter argues for the use of ‘unusual’ theories in psychobiographical research through the presentation of a case study using such a theory. Historically, psychobiographical research has predominantly made use of the work of psychoanalytic and psychodynamic theorists and developmental theorists, while more recent psychobiographical approaches have preferred more modern, empirically based. However, over reliance on a few theories within psychobiographical research creates the possibility for narrow explanations of complex lives. Given the proliferation of theoretical modes in psychology the current use of theory barely scratches the surface of available explanatory paradigms. This chapter argues for the value of casting the explanatory net wider, and for the inclusion of more psychological theories in psychobiographical work. Using a psychobiographical case study, the chapter illustrates how a ‘forgotten’ psychological theory (script theory, based on the work of Tomkins) can serve as an extremely useful explanatory paradigm for a complex religious figure. The case study focuses on Gordon Hinckley (b. 1910, d. 2008), the fifteenth president of The Church of Jesus Christ of Latter-Day Saints (commonly referred to as the Mormon Church), who remains a prominent figure in contemporary Mormonism and played a key role in the rapid growth and increasingly positive public profile of the Religion throughout the twentieth and twenty-first centuries. Using Tomkins’ script theory in conjunction with a psychobiographical method and the analysis of data gathered from published speeches, this study explores Hinckley’s personality structure and identifies three core psychological scripts

    Lawson criterion for ignition exceeded in an inertial fusion experiment

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    For more than half a century, researchers around the world have been engaged in attempts to achieve fusion ignition as a proof of principle of various fusion concepts. Following the Lawson criterion, an ignited plasma is one where the fusion heating power is high enough to overcome all the physical processes that cool the fusion plasma, creating a positive thermodynamic feedback loop with rapidly increasing temperature. In inertially confined fusion, ignition is a state where the fusion plasma can begin "burn propagation" into surrounding cold fuel, enabling the possibility of high energy gain. While "scientific breakeven" (i.e., unity target gain) has not yet been achieved (here target gain is 0.72, 1.37 MJ of fusion for 1.92 MJ of laser energy), this Letter reports the first controlled fusion experiment, using laser indirect drive, on the National Ignition Facility to produce capsule gain (here 5.8) and reach ignition by nine different formulations of the Lawson criterion

    A gravitational-wave standard siren measurement of the Hubble constant

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    The detection of GW170817 (ref. 1) heralds the age of gravitational-wave multi-messenger astronomy, with the observations of gravitational-wave and electromagnetic emission from the same transient source. On 17 August 2017 the network of Advanced Laser Interferometer Gravitational-wave Observatory (LIGO)2 and Virgo3 detectors observed GW170817, a strong signal from the merger of a binary neutron-star system. Less than two seconds after the merger, a γ-ray burst event, GRB 170817A, was detected consistent with the LIGO–Virgo sky localization region4–6). The sky region was subsequently observed by optical astronomy facilities7, resulting in the identification of an optical transient signal within about 10 arcseconds of the galaxy NGC 4993 (refs 8–13). GW170817 can be used as a standard siren14–18, combining the distance inferred purely from the gravitational-wave signal with the recession velocity arising from the electromagnetic data to determine the Hubble constant. This quantity, representing the local expansion rate of the Universe, sets the overall scale of the Universe and is of fundamental importance to cosmology. Our measurements do not require any form of cosmic ‘distance ladder’19; the gravitational-wave analysis directly estimates the luminosity distance out to cosmological scales. Here we report H0 = kilometres per second per megaparsec, which is consistent with existing measurements20,21, while being completely independent of them

    The bii4africa dataset of faunal and floral population intactness estimates across Africa's major land uses

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    This is the final version. Available on open access from Nature Research via the DOI in this recordCode availability: R code for calculating aggregated intactness scores for a focal region (e.g., ecoregion or country) and/or taxonomic group can be downloaded with the bii4africa dataset on Figshare; see Data Records section.Sub-Saharan Africa is under-represented in global biodiversity datasets, particularly regarding the impact of land use on species' population abundances. Drawing on recent advances in expert elicitation to ensure data consistency, 200 experts were convened using a modified-Delphi process to estimate 'intactness scores': the remaining proportion of an 'intact' reference population of a species group in a particular land use, on a scale from 0 (no remaining individuals) to 1 (same abundance as the reference) and, in rare cases, to 2 (populations that thrive in human-modified landscapes). The resulting bii4africa dataset contains intactness scores representing terrestrial vertebrates (tetrapods: ±5,400 amphibians, reptiles, birds, mammals) and vascular plants (±45,000 forbs, graminoids, trees, shrubs) in sub-Saharan Africa across the region's major land uses (urban, cropland, rangeland, plantation, protected, etc.) and intensities (e.g., large-scale vs smallholder cropland). This dataset was co-produced as part of the Biodiversity Intactness Index for Africa Project. Additional uses include assessing ecosystem condition; rectifying geographic/taxonomic biases in global biodiversity indicators and maps; and informing the Red List of Ecosystems.Jennifer Ward Oppenheimer Research Gran

    Multi-messenger Observations of a Binary Neutron Star Merger

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    On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ∌ 1.7 {{s}} with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of {40}-8+8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 {M}ÈŻ . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ∌ 40 {{Mpc}}) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∌10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ∌ 9 and ∌ 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.</p
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