Single Chain Structure of a Poly(<i>N</i>-isopropylacrylamide) Surfactant in Water

Abbott, Lauren J.; Tucker, Ashley K.; Stevens, Mark J.

doi:10.1021/jp511398q

Cited by 65 publications

(82 citation statements)

References 65 publications

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“…For the r-process elements, an extremely neutron-rich environment is requested and in literature several production sites have been proposed. After the detection of the gravitational wave transient GW170817 (Abbott et al 2017), neutron star mergers were greatly supported as production sites for r-process elements, but they might not be the only source (Côté et al 2019and Bonetti et al 2019. In literature, the first production sites proposed were core-collapse SNe (CC SNe) or electron-capture SNe (EC SNe) (Truran 1981;Cowan et al 1991).…”

Section: Introductionmentioning

confidence: 99%

Modelling the chemical evolution of Zr, La, Ce, and Eu in the Galactic discs and bulge

Grisoni

Cescutti

Matteuccí

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We study the chemical evolution of Zr, La, Ce and Eu in the Milky Way discs and bulge by means of chemical evolution models compared with spectroscopic data. We consider detailed chemical evolution models for the Galactic thick disc, thin disc and bulge, which have been already tested to reproduce the observed [α/Fe] vs. [Fe/H] diagrams and metallicity distribution functions for the three different components, and we apply them to follow the evolution of neutron capture elements. In the [Eu/Fe] vs. [Fe/H] diagram, we observe and predict three distinct sequences corresponding to the thick disc, thin disc and bulge, similarly to what happens for the α-elements. We can nicely reproduce the three sequences by assuming different timescales of formation and star formation efficiencies for the three different components, with the thin disc forming on a longer timescale of formation with respect to the thick disc and bulge. On the other hand, in the [X/Fe] vs. [Fe/H] diagrams for Zr, La and Ce, the three populations are mixed and also from the model point of view there is an overlapping between the predictions for the different Galactic components, but the observed behaviour can be also reproduced by assuming different star formation histories in the three components. In conclusions, it is straightforward to see how different star formation histories can lead to different abundance patterns and also looking at the abundance patterns of neutron capture elements can help in constraining the history of formation and evolution of the major Galactic components.

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Section: Introductionmentioning

confidence: 99%

Modelling the chemical evolution of Zr, La, Ce, and Eu in the Galactic discs and bulge

Grisoni

Cescutti

Matteuccí

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…GRB 170817A is a short GRBs associated with the gravitational wave event (GW170817) from the double NS merger which was recently detected by Fermi/GBM (Abbott et al 2017;Goldstein et al 2017). An analysis of the prompt emission of GRB 170817A shows that it consists of two different components.…”

Section: Grb 170817a In Comparison To Short Grbs With Eementioning

confidence: 99%

“…Moreover, the peak flux of both the hard spike and EE of GRB 170817A are smallest out of all our samples. The possible reason may be that GRB 170817A is an off-axis observation (Abbott et al 2017;Alexander et al 2018;Biehl et al2018;Ioka & Nakamura 2019).…”

Section: Grb 170817a In Comparison To Short Grbs With Eementioning

confidence: 99%

“…More interestingly, the short GRB 170817A associated with the gravitational wave event (GW 170817) from double a NS merger was recently detected by Fermi/GBM (Abbott et al 2017;Goldstein et al 2017), and was found to have a prompt emission that is composed of a hard spike of 0.8 s and a weak tail of up to 2.3 s (Goldstein et al 2017;Zhang et al 2018;Pozanenko et al 2018). An interesting question is whether or not GRB 170817A differs in its spectral properties from other typical short GRBs with EE.…”

Section: Introductionmentioning

confidence: 99%

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The properties of prompt emission in short gamma-ray bursts with extended emission observed by Fermi/GBM

Lin

Lü

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Short GRBs with extended emission (EE) that are composed initially of a short-hard spike and followed by a long-lasting EE, are thought to be classified as a subsection of short GRBs. The narrow energy band available during the Swift era combined with a lack of spectral information prevented discovery of the intrinsic properties of those events. In this paper, we performed a systematic search of short GRBs with EE by using all available Fermi/GBM data. The search identified 26 GBM-detected short GRBs with EE that are similar to GRB 060614 observed by Swift/BAT. We focus on investigating the spectral and temporal properties for both the hard spike and the EE components of all 26 GRBs, and explore differences and possible correlations between them. We find that while the peak energy (E p ) of the hard spikes is a little bit harder than that of the EE, but their fluences are comparable. The harder E p seems to correspond to a larger fluence and peak flux with a large scatter for both the hard spike and EE components. Moreover, the E p of both the hard spikes and EE are compared to other short GRBs. Finally, we also compare the properties of GRB 170817A with those short GRBs with EE and find no significant statistical differences between them. We find that GRB 170817A has the lowest E p , likely because it was off-axis. c 0000 RAS 1 CTIME and CSPEC data are not used in our analysis due to the fixed time resolution of 64 ms and 1.024 s, respectively. 2 http://fermi.gsfc.nasa.gov/ssc/data/. 3 http://sourceforge.net/projects/gtburst/. c 0000 RAS, MNRAS 000, 000-000

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“…On 17 August 2017, the LIGO-Virgo network detected a gravitational wave (GW) signal GW170817 from a merging NSB (Abbott et al 2017a). Soon after the detection, associated electromagnetic signals have been extensively observed in various bands and epochs (Abbott et al 2017b).…”

Section: Introductionmentioning

confidence: 99%

Search for neutron star binaries in the Local Group galaxies using LISA

Seto

2019

Monthly Notices of the Royal Astronomical Society

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We discuss the prospects of LISA for detecting neutron star binaries (NSBs) in the local group galaxies such as LMC and M31. Using the recently estimated merger rate 1540 Gpc −3 yr −1 and inversely applying the conventional arguments based on the Bband galaxy luminosities, we estimate the frequency distributions of NSBs in the local galaxies. We find that, after 10 year observation with its current design sensitivity, LISA might detect ∼ 5 NSBs both in LMC and M31 with signal-to-noise ratios larger than 10. Some of the NSBs might be three-dimensionally localized well within LMC. These binaries will be useful for studying various topics including the origin of r-process elements.

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Single Chain Structure of a Poly(N-isopropylacrylamide) Surfactant in Water

Cited by 65 publications

References 65 publications

Modelling the chemical evolution of Zr, La, Ce, and Eu in the Galactic discs and bulge

Modelling the chemical evolution of Zr, La, Ce, and Eu in the Galactic discs and bulge

The properties of prompt emission in short gamma-ray bursts with extended emission observed by Fermi/GBM

Search for neutron star binaries in the Local Group galaxies using LISA

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