Simultaneous Triggered Collapse of the Presolar Dense Cloud Core and Injection of Short-Lived Radioisotopes by a Supernova Shock Wave

Boss, Alan P.; Ипатов, С. И.; Keiser, Sandra A.; Myhill, Elizabeth A.; Vanhala, H. A. T.

doi:10.1086/593057

Cited by 73 publications

(94 citation statements)

References 24 publications

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“…However, these models led to considerably lower injection efficiencies than those previously estimated on the basis of models where the shock-cloud interaction was assumed to be isothermal (Boss 1995;Foster & Boss 1997;Vanhala & Boss 2002). When the injection efficiency (f i ) is defined to be the fraction of the incident shock wave material that is injected into the collapsing cloud core, values of f i ∼ 0.001 result from the nonisothermal models (Boss et al 2008(Boss et al , 2010, about 100 times lower than the values of f i found previously for strictly isothermal interactions.…”

Section: Introductionmentioning

confidence: 89%

“…Recent calculations have shown that simultaneously triggered gravitational collapse and injection of shock wave gas and dust into the collapsing cloud core is possible even when detailed heating and cooling processes in the shock-cloud interaction are included (Boss et al 2008). Shock speeds in the range from 5 km s −1 to 70 km s −1 are capable of achieving simultaneous triggering and injection for a 2.2 M target cloud (Boss et al 2010).…”

Section: Introductionmentioning

confidence: 99%

“…Considering that the shock fronts in these models contain 0.015 M of gas and dust, this means that the Boss et al (2008Boss et al ( , 2010) models produced nominal dilution factors D ∼ 10 −5 , where D is defined as the ratio of the amount of mass derived from the stellar source of the shock front that ends up in the protoplanetary disk to the amount of mass in the disk that did not derive from the stellar source. Such values appear to be much too low to explain the initial abundances inferred for typical SLRIs, which range from ∼10 −4 to ∼3 × 10 −3 for supernovae (Takigawa et al 2008;Gaidos et al 2009) and ∼3 × 10 −3 for an AGB star (Trigo-Rodríguez et al 2009).…”

Section: Introductionmentioning

confidence: 99%

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Who Pulled the Trigger: A Supernova or an Asymptotic Giant Branch Star?

Boss

Keiser

2010

ApJ

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The short-lived radioisotope (SLRI) 60 Fe requires production in a core collapse supernova or asymptotic giant branch (AGB) star immediately before its incorporation into the earliest solar system solids. Shock waves from a somewhat distant supernova, or a relatively nearby AGB star, have the right speeds to simultaneously trigger the collapse of a dense molecular cloud core and to inject shock wave material into the resulting protostar. A new set of FLASH2.5 adaptive mesh refinement hydrodynamic models shows that the injection efficiency depends sensitively on the assumed shock thickness and density. Supernova shock waves appear to be thin enough to inject the amount of shock wave material necessary to match the SLRI abundances measured for primitive meteorites. Planetary nebula shock waves from AGB stars, however, appear to be too thick to achieve the required injection efficiencies. These models imply that a supernova pulled the trigger that led to the formation of our solar system.

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Section: Introductionmentioning

confidence: 89%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Who Pulled the Trigger: A Supernova or an Asymptotic Giant Branch Star?

Boss

Keiser

2010

ApJ

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“…First, a supernova explosion might have triggered collapse of a pre-stellar gas core a few pc away, leading to formation of the Sun in a gas cloud that has just been enriched by supernova ejecta (e.g. Boss et al 2008). If this scenario is correct, then we have little hope of finding the Sun's siblings, because the supernova that injected the nuclides would also lead to significant chemical inhomogeneity in the Sun's parent cluster.…”

Section: The Solar Familymentioning

confidence: 99%

The Long-Term Evolution of the Galactic Disk Traced by Dissolving Star Clusters

Bland-Hawthorn

Krumholz

Freeman

2010

ApJ

173

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The Galactic disk retains a vast amount of information about how it came to be, and how it evolved over cosmic time. However, we know very little about the secular processes associated with disk evolution. One major uncertainty is the extent to which stars migrate radially through the disk, thereby washing out signatures of their past (e.g. birth sites). Recent theoretical work finds that such "blurring" of the disk can be important if spiral arms are transient phenomena. Here we describe an experiment to determine the importance of diffusion from the Solar circle with cosmic time. Consider a star cluster that has been placed into a differentially rotating, stellar fluid. We show that all clusters up to ∼ 10 4 M in mass, and a significant fraction of those up to ∼ 10 5 M , are expected to be chemically homogeneous, and that clusters of this size can be assigned a unique "chemical tag" by measuring the abundances of 10 independent element groups, with better age and orbit determinations allowing fewer abundance measurements. The star cluster therefore acts like a "tracer dye", and the present-day distribution of its stars provides a strong constraint on the rate of radial diffusion or migration in the Galactic disk. A star cluster of particular interest for this application is the "Solar family" − the stars that were born with the Sun. If we were able to identify a significant fraction of these, we could determine whether the Sun was born at its present radius or much further in. We show all-sky projections for the Solar Family under different dynamical scenarios and identify the most advantageous fields on the sky for the experiment. Sellwood & Binney have argued for strong radial transport driven by transient spiral perturbations: in principle, we could measure the strength of this migration directly. In searching for the Solar family, we would also identify many thousands of other chemically homogeneous groups, providing a wealth of additional information. We discuss this prospect in the context of the upcoming HERMES high-resolution million-star survey.

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“…5-10 ms), much shorter than for CVD processes (Battaile et al 1997;Chung and Sung 2001;Aleksandrov and Sel'skaya 2002;Abbashian et al 2005;Mokuno et al 2006;Karczemska et al 2008). According to Boss et al (2008) the speed of the shock wave was calculated in a simulation of the triggered collapse of a presolar dense cloud core. In that case the transition would be 2.6 nm/20 km/sec (=0.13 picoseconds).…”

Section: (Nm)=rd (Nm/s)t (S)mentioning

confidence: 99%

Micro-Raman study of the Allende meteoritic nanodiamonds: Supernova-driven shock wave origin is revisited

Gucsik¹

2011

Central European Geology

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I have studied the Raman spectroscopic signatures of nanodiamonds from the Allende meteorite, in which some portions must be of presolar origin as indicated by the isotopic compositions of various trace elements. The spectra of the meteoritic nanodiamonds show a narrow peak at 1326 cm -1 and a broad band at 1590 cm -1 . Compared to the intensities of these peaks, the background fluorescence is relatively high. A significant frequency shift from 1332 to 1326 cm -1 , peak broadening, and appearance of a new peak at 1590 cm -1 might be due to shock effects during formation of the diamond grains. Such changes may have several origins: an increase in bond length, a change in the electron density function or charge transfer, or a combination of these factors. However, Raman spectroscopy alone does not allow distinguishing between a shock origin of the nanodiamonds and formation by a CVD process, as is favored by most workers.

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Simultaneous Triggered Collapse of the Presolar Dense Cloud Core and Injection of Short-Lived Radioisotopes by a Supernova Shock Wave

Cited by 73 publications

References 24 publications

Who Pulled the Trigger: A Supernova or an Asymptotic Giant Branch Star?

Who Pulled the Trigger: A Supernova or an Asymptotic Giant Branch Star?

The Long-Term Evolution of the Galactic Disk Traced by Dissolving Star Clusters

Micro-Raman study of the Allende meteoritic nanodiamonds: Supernova-driven shock wave origin is revisited

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