Evidence for Nearby Supernova Explosions

Benı́tez, N.; Maíz‐Apellániz, Jesús; Cañelles, Matilde

doi:10.1103/physrevlett.88.081101

Cited by 98 publications

(157 citation statements)

References 40 publications

(71 reference statements)

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“…The presence of a nearby SN explosion was previously noticed in a completely different type of data on abun-dance of isotopes on Earth [36][37][38][39]. These data suggest that an episode of deposition of 60 Fe isotopes in the million years old deep ocean crust was produced by the passage of an expanding shell of a 2 Myr old supernova remnant through the Solar System.…”

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confidence: 74%

Signatures of a Two Million Year Old Supernova in the Spectra of Cosmic Ray Protons, Antiprotons, and Positrons

2015

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The locally observed cosmic ray spectrum has several puzzling features, such as the excess of positrons and antiprotons above ∼ 20 GeV and the discrepancy in the slopes of the spectra of cosmic ray protons and heavier nuclei in the TeV-PeV energy range. We show that these features are consistently explained by a nearby source which was active ∼ 2 Myr ago and has injected (2 − 3) × 10 50 erg in cosmic rays. The transient nature of the source and its overall energy budget point to the supernova origin of this local cosmic ray source. The age of the supernova suggests that the local cosmic ray injection was produced by the same supernova that has deposited 60 Fe isotopes in the deep ocean crust.

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confidence: 74%

Signatures of a Two Million Year Old Supernova in the Spectra of Cosmic Ray Protons, Antiprotons, and Positrons

2015

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“…The best candidate would be a shock wave produced by a very recent and nearby stellar explosion, because there is no evidence of either a spectral index change or a cutoff in the electron spectrum up to 1-2 TeV. Hence, the source might be the last stellar collapse among the supernovae that formed the local bubble ( Erlykin & Wolfendale 1997;Maíz-Apellániz 2001;Benítez et al 2002).…”

Section: Discussionmentioning

confidence: 99%

The Origin of Cosmic Ray Electrons and Positrons

Casadei

Bindi

2004

ApJ

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We use direct measurements of electrons and positrons corrected for solar modulation in the force-field approximation to obtain estimations of the local interstellar spectra. The resulting overall electron spectrum fits well with a single power law above a few GeV with spectral index À ¼ 3:44 AE 0:03, consistent with the spectral index obtained for the positron spectrum þ ¼ 3:43 AE 0:05, therefore suggesting a common acceleration process for both species. We propose that the acceleration engine was a nearby and recent shock wave originating from the last supernova explosion among those that formed the local bubble. This shock wave had to be quite soft, because no effect is seen on the proton spectrum. However, the large spread between different experiments clearly suggests the need for new, accurate measurements over a large energy range.

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“…On the other hand, Type II SNe are expected to account for only 30% of the total yield of Fe (Matteucci & Greggio 1986) but are expected to do so on a shorter timescale (3−5 Myr). A high rate of local SN type II explosions has been estimated to explain the local bubble (Maíz-Apellániz 2001), namely 20 SN type II explosions within 150 pc of the Sun in the past 11 Myr (Benítez et al 2002). The youngest stars in the SWD and SWOD samples have ages of 15 Myr and 35 Myr, respectively, with a larger number of young SWDs in the first 500 Myr bin.…”

Section: Possible Biasesmentioning

confidence: 99%

Metallicity of solar-type stars with debris discs and planets

Maldonado

Eiroa

Villaver

et al. 2012

A&A

100

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Context. Around 16% of the solar-like stars in our neighbourhood show IR-excesses due to dusty debris discs and a fraction of them are known to host planets. Determining whether these stars follow any special trend in their properties is important to understand debris disc and planet formation. Aims. We aim to determine in a homogeneous way the metallicity of a sample of stars with known debris discs and planets. We attempt to identify trends related to debris discs and planets around solar-type stars. Methods. Our analysis includes the calculation of the fundamental stellar parameters T eff , log g, microturbulent velocity, and metallicity by applying the iron ionisation equilibrium conditions to several isolated Fe i and Fe ii lines. High-resolution échelle spectra (R ∼ 57 000) from 2, 3 m class telescopes are used. Our derived metallicities are compared with other results in the literature, which finally allows us to extend the stellar samples in a consistent way. Results. The metallicity distributions of the different stellar samples suggest that there is a transition toward higher metallicities from stars with neither debris discs nor planets to stars hosting giant planets. Stars with debris discs and stars with neither debris nor planets follow a similar metallicity distribution, although the distribution of the first ones might be shifted towards higher metallicities. Stars with debris discs and planets have the same metallicity behaviour as stars hosting planets, irrespective of whether the planets are low-mass or gas giants. In the case of debris discs and giant planets, the planets are usually cool, -semimajor axis larger than 0.1 AU (20 out of 22 planets), even ≈65% have semimajor axis larger than 0.5 AU. The data also suggest that stars with debris discs and cool giant planets tend to have a low dust luminosity, and are among the less luminous debris discs known. We also find evidence of an anticorrelation between the luminosity of the dust and the planet eccentricity. Conclusions. Our data show that the presence of planets, not the debris disc, correlates with the stellar metallicity. The results confirm that core-accretion models represent suitable scenarios for debris disc and planet formation. These conclusions are based on a number of stars with discs and planets considerably larger than in previous works, in particular stars hosting low-mass planets and debris discs. Dynamical instabilities produced by eccentric giant planets could explain the suggested dust luminosity trends observed for stars with debris discs and planets.

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Evidence for Nearby Supernova Explosions

Cited by 98 publications

References 40 publications

Signatures of a Two Million Year Old Supernova in the Spectra of Cosmic Ray Protons, Antiprotons, and Positrons

Signatures of a Two Million Year Old Supernova in the Spectra of Cosmic Ray Protons, Antiprotons, and Positrons

The Origin of Cosmic Ray Electrons and Positrons

Metallicity of solar-type stars with debris discs and planets

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