Supernova ejecta in ocean cores used as time constraints for nearby stellar groups

Hyde, Megan; Pecaut, Mark J.

doi:10.1002/asna.201713375

Cited by 12 publications

(13 citation statements)

References 37 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…More precise estimate would increase the energy by at least 10 if radiation losses are taken into account (see Figure 1) provided the energy is injected by explosions. 1 Similar estimate is obtained recently from a detailed analysis of Sco-Cen star formation history [31]. The volume filling factor of gas with given temperatures (see legend) for the same SN rates.…”

Section: Local Hot Bubble and The Supershell From Sco-censupporting

confidence: 66%

Multi-Wavelength Observations and Modeling of Loop I

Shchekinov

2018

Galaxies

View full text Add to dashboard Cite

The article aims to overview the origin and current dynamical state of a giant structure on the northern galactic sky—the radio Loop I extending from ≈ − 45 ∘ to ≈ + 45 ∘ in longitudes and up to ≈ 80 ∘ in latitudes over the Galactic center (GC). The main issue addressed here is a description of possible sources of mass and energy able to build up the Loop I and associated structures seen in X-ray, 21 cm, far infrared (FIR), and maintain them on long timescales. This region of the sky is highly crowded, such that contaminations from many projected structures can be tangled, and not always current direct observations look sufficient to disentangle them. At such conditions indirect arguments based on analysis of underlying star formation (SF) rate, morphological features in radio, X-ray and FIR may be important for understanding the origin of Loop I. Simple estimates show that the observed rather weak SF rate is able to create and maintain Loop I, and under certain circumstances can provide the observed east-west asymmetry. However, an explanation of an apparent coexistence of morphologically similar HI and FIR filaments close to Loop I is challenging, indicating that most likely they may belong to the foreground. Recently discovered absorptions in diffuse interstellar bands seem to confirm this picture.

show abstract

Section: Local Hot Bubble and The Supershell From Sco-censupporting

confidence: 66%

Multi-Wavelength Observations and Modeling of Loop I

Shchekinov

2018

Galaxies

View full text Add to dashboard Cite

show abstract

“…However, there are several problems in the B16 model, apart from the fact that B16 assumed that all 16 missing stars exploded as SN, while one or two most massive ones could have formed Black Holes, and a few should be ejected runaways: (i) The most likely masses of the missing stars fix the lifetimes until their SNe. However, because the association age of ∼ 22.5 Myr assumed in B16 is higher than ∼ 10 − 20 Myr (see footnote 1), the lower-mass SN progenitors, up to roughly 13-14 M (Ekström et al 2012), have not exploded, yet, even for a large age spread: there is no evidence that the lowest-mass SN progenitors would form first (Pecaut & Mamajek 2016, Hyde & Pecaut 2018. The more massive stars exploded in the last ∼ 6 − 7 Myr yielding sufficient 60 Fe, as detected on Earth.…”

Section: Discussion Of the Breitschwerdt Et Al (2016) Modelmentioning

confidence: 95%

“…4). While Tucana-Horologium (Tuc-Hor) has also been suggested as possible site of a nearby recent SN (Mamajek 2016, Hyde & Pecaut 2018), Scorpius-Centaurus-Lupus is a priori more likely, because it contains many more massive stars.…”

Section: Introduction: 60 Fe On Earthmentioning

confidence: 99%

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Neuhäuser

Gießler

Hambaryan

2019

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

The detection of ∼ 1.5−3.2 Myr old 60 Fe on Earth indicates recent nearby core-collapse supernovae. For supernovae in multiple stars, the primary stars may become neutron stars, while former companions may become unbound and become runaway stars. We wrote software for tracing back the space motion of runaway and neutron stars to young associations of massive stars. We apply it here to the nearby young Scorpius-Centaurus-Lupus groups, all known runaway stars possibly coming from there, and all 400 neutron stars with known transverse velocity. We find kinematic evidence that the runaway ζ Oph and the radio pulsar PSR B1706-16 were released by a supernova in a binary 1.78 ± 0.21 Myr ago at 107 ± 4 pc distance (for pulsar radial velocity 260 ± 43 km/s); association age and flight time determine the progenitor mass (16-18 M ), which can constrain supernova nucleosynthesis yields and 60 Fe uptake on Earth. In addition, we notice that the only high-mass X-ray binary in Scorpius-Centaurus-Lupus (1H11255-567 with µ 1 and µ 2 Cru) may include a neutron star formed in another SN, up to ∼ 1.8 Myr ago at 89 − 112 pc, i.e. also yielding 60 Fe detectable on Earth. Our scenario links 60 Fe found on Earth to one or two individual supernovae in multiple stars.

show abstract

“…A direct detection of 60 Fe nuclei in Galactic cosmic rays also supports a recent near-Earth SN within a few Myr (Binns et al 2016). The ScorpiusâĂŞCentaurus OB association and the Tucana-Horologium OB association have been suggested as a possible source of the 60 Fe-producing SNe (Breitschwerdt et al 2016;Schulreich et al 2017;Hyde & Pecaut 2018). Moreover, a detection of 60 Fe in Antarctic snow shows that delivery of this isotope was not limited to a single event in the geologic past.…”

Section: Introductionmentioning

confidence: 62%

Formation and evolution of the local interstellar environment: combined constraints from nucleosynthetic and X-ray data

Fujimoto,

Krumholz,

Inutsuka

et al. 2020

Preprint

View full text Add to dashboard Cite

Several observations suggest that the Solar system has been located in a region affected by massive stellar feedback for at least a few Myr; these include detection of live 60 Fe in deep-sea archives and Antarctic snow, the broad angular distribution of 26 Al around the Galactic plane seen in all-sky γ-ray maps, and the all-sky soft X-ray background. However, our position inside the Galactic disc makes it difficult to fully characterise this environment, and our limited time baseline provides no information about its formation history or relation to large-scale Galactic dynamics. We explore these questions by using an N-body+hydrodynamics simulation of a Milky-Way-like galaxy to identify stars on Sun-like orbits whose environments would produce conditions consistent with those we observe. We find that such stars are uncommon but not exceptionally rare. These stars are found predominantly near the edges of spiral arms, and lie inside kpc-scale bubbles that are created by multiple generations of star formation in the arm. We investigate the stars' trajectories and find that the duration of the stay in the bubble ranges from 20 Myr to 90 Myr. The duration is governed by the crossing time of stars across the spiral arm. This is generally shorter than the bubble lifetime, which is∼ 100 Myr as a result of the continuous gas supply provided by the arm environment.

show abstract

Supernova ejecta in ocean cores used as time constraints for nearby stellar groups

Cited by 12 publications

References 37 publications

Multi-Wavelength Observations and Modeling of Loop I

Multi-Wavelength Observations and Modeling of Loop I

A nearby recent supernova that ejected the runaway star ζ Oph, the pulsar PSR B1706−16, and 60Fe found on Earth

Formation and evolution of the local interstellar environment: combined constraints from nucleosynthetic and X-ray data

Contact Info

Product

Resources

About