Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source?

Busso, M.; Gallino, R.; Wasserburg, G. J.

doi:10.1071/as03035

Cited by 55 publications

(79 citation statements)

References 134 publications

(231 reference statements)

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“…Note that in our earlier work [97] we gave q I He /q I 0 and (N R /N I ) He in the production shells. Here we explicitly calculated the values of N R /N I and q I EN V /q I 0 in the envelope over the evolution of the star as done in [58] [201]. The values of q I EN V /q I 0 are presented in Table 3 and are shown in Fig.…”

Section: What Do Agb Stars Produce?mentioning

confidence: 99%

“…A critical matter will be the nature of nucleosynthetic yields of potential sources. A recent review of the short-lived nuclei by Busso et al [58] will be used as the source for the present report. Substantial new results will be presented concerning the characteristics of AGB stars of a range in masses and with specific consideration of the results of cool bottom processing (see Section 4).…”

Section: Introductionmentioning

confidence: 99%

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Short-lived nuclei in the early Solar System: Possible AGB sources

et al. 2006

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The abundances of short-lived radionuclides in the early solar system (ESS) are reviewed, as well as the methodology used in determining them. These results are compared with the inventory estimated for a uniform galactic production model. It is shown that, to within a factor of two, the observed abundances of 238 U, 235 U, 232 Th, 244 Pu, 182 Hf, 146 Sm, and 53 Mn are roughly compatible with long-term galactic nucleosynthesis. 129 I is an exception, with an ESS inventory much lower than expected from uniform production. The isotopes 107 Pd, 60 Fe, 41 Ca, 36 Cl, 26 Al, and 10 Be require late addition to the protosolar nebula. 10 Be is the product of energetic particle irradiation of the solar system as most probably is 36 Cl. Both of these nuclei appear to be present when 26 Al is absent. A late injection by a supernova (SN) cannot be responsible for most of the short-lived nuclei without excessively producing 53 Mn; it can however be the source of 53 Mn itself and possibly of 60 Fe. If a late SN injection is responsible for these two nuclei, then there remains the problem of the origin of 107 Pd and several other isotopes. Emphasis is given to an AGB star as a source of many of the nuclei, including 60 Fe; this possibility is explored with a new generation of stellar models. It is shown that if the dilution factor (i.e. the ratio of the contaminating mass to the solar parental cloud mass) is f 0 ∼ 4×10 −3 , a reasonable representation for many nuclei is obtained; this requires that ( 60 Fe/ 56 Fe) ESS ∼ 10 −7 to 2×10 −6 . The nuclei produced by an AGB source do not include 53 Mn, 10 Be or 36 Cl if it is very abundant. The role of irradiation is discussed with regard to 26 Al, 36 Cl and 41 Ca, and the estimates of bulk solar abundances of these isotopes are commented on. The conflict between various scenarios is emphasized as well as the current absence of an astrophysically plausible global interpretation for all the existing data. Examination of abundances for the actinides indicates that a quiescent interval of ∼ 10 8 years is required for actinide group production. This is needed in order to explain the data on 244 Pu and the new bounds on 247 Cm. Because this quiescent interval is not compatible with the 182 Hf data, a separate type of r-process event is needed for at least the actinides, distinct from the two types that have previously been identified. The apparent coincidence of the 129 I and trans-actinide time scales suggests that the last heavy r contribution was from an r-process that produced very heavy nuclei but without fission recycling so that the yields at Ba and below (including I) were governed by fission.

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Section: What Do Agb Stars Produce?mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Short-lived nuclei in the early Solar System: Possible AGB sources

et al. 2006

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“…Ellis et al (1996) identified several possible target isotopes for such a study, including 60 Fe (see also Korschinek et al 1996), which is believed to be produced primarily in core-collapse and electroncapture SNe of massive stars, with mass M 8 M , via successive neutron capture on preexisting Fe isotopes, both before and during the explosion (Timmes et al 1995;Wanajo et al 2013). Other suggested sources are asymptotic giant branch (AGB; Busso et al 2003) and super-AGB (SAGB; Lugaro et al 2012) stars, as well as a rare class of high-density thermonuclear SNe (Woosley 1997).…”

Section: Introductionmentioning

confidence: 99%

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

Schulreich

Breitschwerdt

Feige

et al. 2017

A&A

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Context. The discovery of radionuclides like 60 Fe with half-lives of million years in deep-sea crusts and sediments offers the unique possibility to date and locate nearby supernovae. Aims. We want to quantitatively establish that the 60 Fe enhancement is the result of several supernovae which are also responsible for the formation of the Local Bubble, our Galactic habitat. Methods. We performed three-dimensional hydrodynamic adaptive mesh refinement simulations (with resolutions down to subparsec scale) of the Local Bubble and the neighbouring Loop I superbubble in different homogeneous, self-gravitating environments. For setting up the Local and Loop I superbubble, we took into account the time sequence and locations of the generating core-collapse supernova explosions, which were derived from the mass spectrum of the perished members of certain stellar moving groups. The release of 60 Fe and its subsequent turbulent mixing process inside the superbubble cavities was followed via passive scalars, where the yields of the decaying radioisotope were adjusted according to recent stellar evolution calculations. Results. The models are able to reproduce both the timing and the intensity of the 60 Fe excess observed with rather high precision, provided that the external density does not exceed 0.3 cm −3 on average. Thus the two best-fit models presented here were obtained with background media mimicking the classical warm ionised and warm neutral medium. We also found that 60 Fe (which is condensed onto dust grains) can be delivered to Earth via two physical mechanisms: either through individual fast-paced supernova blast waves, which cross the Earth's orbit sometimes even twice as a result of reflection from the Local Bubble's outer shell, or, alternatively, through the supershell of the Local Bubble itself, injecting the 60 Fe content of all previous supernovae at once, but over a longer time range.

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“…These findings have motivated two different kinds of explanations. The external model stipulates that the radionuclides were made in a supernova or in an asymptotic giant branch (AGB) star (e.g., Busso et al 2003). In the case of a supernova, it has been proposed that the expelled material triggered the collapse of a nearby molecular cloud core, which led to the formation of the solar system (Cameron & Truran 1977 ).…”

Section: Introductionmentioning

confidence: 99%

The Irradiation Origin of Beryllium Radioisotopes and Other Short‐lived Radionuclides

Gounelle

Shu

Shang

et al. 2006

ApJ

122

140

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Two explanations exist for the short-lived radionuclides (T 1/2 5 Myr) present in the solar system when the calcium-aluminum-rich inclusions (CAIs) first formed. They originated either from the ejecta of a supernova or by the in situ irradiation of nebular dust by energetic particles. With a half-life of only 53 days, 7 Be is then the key discriminant, since it can be made only by irradiation. Using the same irradiation model developed earlier by our group, we calculate the yield of 7 Be. Within model uncertainties associated mainly with nuclear cross sections, we obtain agreement with the experimental value. Moreover, if 7 Be and 10 Be have the same origin, the irradiation time must be short (a few to tens of years), and the proton flux must be of order F $ 2 ; 10 10 cm À2 s À1 . The X-wind model provides a natural astrophysical setting that gives the requisite conditions. In the same irradiation environment, 26 Al, 36 Cl, and 53 Mn are also generated at the measured levels within model uncertainties, provided that irradiation occurs under conditions reminiscent of solar impulsive events (steep energy spectra and high 3 He abundance). The decoupling of the 26 Al and 10 Be observed in some rare CAIs receives a quantitative explanation when rare gradual events (shallow energy spectra and low 3 He abundance) are considered. The yields of 41 Ca are compatible with an initial solar system value inferred from the measured initial 41 Ca / 40 Ca ratio and an estimate of the thermal metamorphism time (from Young et al.), alleviating the need for two-layer proto-CAIs. Finally, we show that the presence of supernova-produced 60 Fe in the solar accretion disk does not necessarily mean that other short-lived radionuclides have a stellar origin.

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Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source?

Cited by 55 publications

References 134 publications

Short-lived nuclei in the early Solar System: Possible AGB sources

Short-lived nuclei in the early Solar System: Possible AGB sources

Numerical studies on the link between radioisotopic signatures on Earth and the formation of the Local Bubble

The Irradiation Origin of Beryllium Radioisotopes and Other Short‐lived Radionuclides

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