Astrophysical neutrinos

Ruderman, M.

doi:10.1088/0034-4885/28/1/312

Cited by 31 publications

(9 citation statements)

References 76 publications

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“…The existence of burst oscillations indicates that the emission from the surface, and hence the thermonuclear burning, is not uniform over the entire star. This is in accord with theoretical expectations (Joss 1978;Ruderman 1981;Shara 1982;Livio & Bath 1982;Fryxell & Woosley 1982;Nozakura, Ikeuchi, & Fujimoto 1984;Bildsten 1995), and it suggests that the properties of the burst oscillations, such as the evolution of their frequency or amplitude, may contain valuable information about the propagation of thermonuclear burning over the surface of the neutron star. The lessons learned from study of the thermonuclear propagation in bursts may ultimately further our understanding of thermonuclear propagation in other astrophysical contexts, such as classical novae and Type Ia supernovae.…”

Section: Introductionsupporting

confidence: 86%

A Characterization of the Brightness Oscillations during Thermonuclear Bursts from 4U 1636−536

Miller

2000

ApJ

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The discovery of nearly coherent brightness oscillations during thermonuclear X-ray bursts from six neutron-star low-mass X-ray binaries has opened up a new way to study the propagation of thermonuclear burning, and may ultimately lead to greater understanding of thermonuclear propagation in other astrophysical contexts, such as in Type Ia supernovae. Here we report detailed analyses of the ∼580 Hz brightness oscillations during bursts from 4U 1636-536. We investigate the bursts as a whole and, in more detail, the initial portions of the bursts. We analyze the ∼580 Hz oscillations in the initial 0.75 seconds of the five bursts that were used in a previous search for a brightness oscillation at the expected ∼290 Hz spin frequency, and find that if the same frequency model describes all five bursts there is insufficient data to require more than a constant frequency or, possibly, a frequency plus a frequency derivative. Therefore, although it is appropriate to use an arbitrarily complicated model of the ∼580 Hz oscillations to generate a candidate waveform for the ∼290 Hz oscillations, models with more than two parameters are not required by the data. For the bursts as a whole we show that the characteristics of the brightness oscillations vary greatly from burst to burst. We find, however, that in at least one of the bursts, and possibly in three of the four that have strong brightness oscillations throughout the burst, the oscillation frequency reaches a maximum several seconds into the burst and then decreases. This behavior has not been reported previously for burst brightness oscillations, and it poses a challenge to the standard burning layer expansion explanation for the frequency changes.

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Section: Introductionsupporting

confidence: 86%

A Characterization of the Brightness Oscillations during Thermonuclear Bursts from 4U 1636−536

Miller

2000

ApJ

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“…Prescient remarks about this potential were made long ago (e.g., [4][5][6][7][8]. As Bahcall wrote in 1964 (9, p. 300) about solar neutrinos, before their detection, "Only neutrinos, with their extremely small interaction cross sections, can enable us to see into the interior of a star and thus verify directly the hypothesis of nuclear energy generation in stars."…”

Section: Impossible Dreams Of Neutrino Astronomymentioning

confidence: 99%

The Diffuse Supernova Neutrino Background

Beacom

2010

Annu. Rev. Nucl. Part. Sci.

293

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The Diffuse Supernova Neutrino Background (DSNB) is the weak glow of MeV neutrinos and antineutrinos from distant core-collapse supernovae. The DSNB has not been detected yet, but the Super-Kamiokande (SK) 2003 upper limit on the electron antineutrino flux is close to predictions, now quite precise, based on astrophysical data. If SK is modified with dissolved gadolinium to reduce detector backgrounds and increase the energy range for analysis, then it should detect the DSNB at a rate of a few events per year, providing a new probe of supernova neutrino emission and the cosmic core-collapse rate. If the DSNB is not detected, then new physics will be required. Neutrino astronomy, while uniquely powerful, has proven extremely difficult -- only the Sun and the nearby Supernova 1987A have been detected to date -- so the promise of detecting new sources soon is exciting indeed.Comment: Submitted to Annual Review of Nuclear and Particle Science, Volume 60. 25 pages with 7 figures

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“…Prescient remarks about this potential were made long ago, e.g., Refs. (4)(5)(6)(7)(8). As Bahcall wrote in 1964 about solar neutrinos, before their detection, "Only neutrinos, with their extremely small interaction cross sections, can enable us to see into the interior of a star..." (9).…”

Section: Impossible Dreams Of Neutrino Astronomymentioning

confidence: 99%

The Diffuse Supernova Neutrino Background

Beacom

2010

Preprint

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The Diffuse Supernova Neutrino Background (DSNB) is the weak glow of MeV neutrinos and antineutrinos from distant core-collapse supernovae. The DSNB has not been detected yet, but the Super-Kamiokande (SK) 2003 upper limit on the νe flux is close to predictions, now quite precise, based on astrophysical data. If SK is modified with dissolved gadolinium to reduce detector backgrounds and increase the energy range for analysis, then it should detect the DSNB at a rate of a few events per year, providing a new probe of supernova neutrino emission and the cosmic core-collapse rate. If the DSNB is not detected, then new physics will be required. Neutrino astronomy, while uniquely powerful, has proven extremely difficultonly the Sun and the nearby Supernova 1987A have been detected to date -so the promise of detecting new sources soon is exciting indeed.

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Astrophysical neutrinos

Cited by 31 publications

References 76 publications

A Characterization of the Brightness Oscillations during Thermonuclear Bursts from 4U 1636−536

A Characterization of the Brightness Oscillations during Thermonuclear Bursts from 4U 1636−536

The Diffuse Supernova Neutrino Background

The Diffuse Supernova Neutrino Background

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