Early Optical Spectra of Nova V1369 Cen Show the Presence of Lithium

Izzo, L.; Valle, M. Della; Mason, E.; Matteuccí, F.; Romano, D.; Pasquini, L.; Vanzi, L.; Jordán, Andrés; Fernández, J. M.; Bluhm, P.; Brahm, R.; Espinoza, N.; Williams, Robert E.

doi:10.1088/2041-8205/808/1/l14

Cited by 102 publications

(138 citation statements)

References 44 publications

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“…They evaluated the mass fraction of 7 Be in the ejecta as X( 7 Be) ∼ 10 −4.3±0.3 . These discoveries show that novae are important production sites of 7 Li nuclei (see also [30][31][32]). Nova eruption occurs when the hydrogen gas accreted onto a white dwarf from its companion star accumulates and undergoes thermonuclear runaways.…”

Section: Introductionmentioning

confidence: 94%

Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

Kawanaka

Yanagita

2018

Phys. Rev. Lett.

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Recent measurements of cosmic-ray light nuclei by AMS-02 have shown that there is an unexpected component of cosmic-ray (CR) lithium whose spectral index is harder than that expected from the secondary production scenario. We propose the nearby Type Ia supernova following a nova eruption as the origin of lithium nuclei in the CRs. By fitting the data of CR protons, helium, and lithium fluxes provided by AMS-02 with our theoretical model we show that this scenario is consistent with the observations. The observational tests that can check our hypothesis are briefly discussed.

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Section: Introductionmentioning

confidence: 94%

Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

Kawanaka

Yanagita

2018

Phys. Rev. Lett.

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“…Novae might also act in the right direction, since they restore the products of explosive H burning on relatively long timescales (see, e.g., Romano et al 1999;Romano & Matteucci 2003, and (José & Hernanz 1998, although the actual yields remain highly uncertain. It is worth remarking that Izzo et al (2015) detected Li expelled by a nova system (see also Tajitsu et al 2015) and found a total amount of Li ejected in a single nova outburst that is significantly larger than expected from hydrodynamic nova models by José & Hernanz (1998). In this context, it would be interesting to investigate whether some extra 23 Na can be produced in these same events in amounts that would reverse the decreasing trend of [Na/Fe] with time predicted by current chemical evolution models (see next section).…”

Section: Trends With Metallicitymentioning

confidence: 99%

TheGaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs

Smiljanić

Romano

Bragaglia

et al. 2016

A&A

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Context. Stellar evolution models predict that internal mixing should cause some sodium overabundance at the surface of red giants more massive than ∼1.5-2.0 M . The surface aluminium abundance should not be affected. Nevertheless, observational results disagree about the presence and/or the degree of Na and Al overabundances. In addition, Galactic chemical evolution models adopting different stellar yields lead to very different predictions for the behavior of [Na/Fe] and [Al/Fe] versus [Fe/H]. Overall, the observed trends of these abundances with metallicity are not well reproduced. Aims. We readdress both issues, using new Na and Al abundances determined within the Gaia-ESO Survey. Our aim is to obtain better observational constraints on the behavior of these elements using two samples: i) more than 600 dwarfs of the solar neighborhood and of open clusters and ii) low-and intermediate-mass clump giants in six open clusters. Methods. Abundances were determined using high-resolution UVES spectra. The individual Na abundances were corrected for nonlocal thermodynamic equilibrium effects. For the Al abundances, the order of magnitude of the corrections was estimated for a few representative cases. For giants, the abundance trends with stellar mass are compared to stellar evolution models. For dwarfs, the abundance trends with metallicity and age are compared to detailed chemical evolution models. Results. Abundances of Na in stars with mass below ∼2.0 M , and of Al in stars below ∼3.0 M , seem to be unaffected by internal mixing processes. For more massive stars, the Na overabundance increases with stellar mass. This trend agrees well with predictions of stellar evolutionary models. For Al, our only cluster with giants more massive than 3.0 M , NGC 6705, is Al enriched. However, this might be related to the environment where the cluster was formed. Chemical evolution models that well fit the observed [Na/Fe] vs. [Fe/H] trend in solar neighborhood dwarfs cannot simultaneously explain the run of [Al/Fe] with [Fe/H], and vice versa. The comparison with stellar ages is hampered by severe uncertainties. Indeed, reliable age estimates are available for only a half of the stars of the sample. We conclude that Al is underproduced by the models, except for stellar ages younger than about 7 Gyr. In addition, some significant source of late Na production seems to be missing in the models. Either current Na and Al yields are affected by large uncertainties, and/or some important Galactic source(s) of these elements has as yet not been taken into account.

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“…Recently, Izzo et al (2015) revealed a "very clear signature" of lithium speeding away from the stellar nova explosion at a speed of two million kilometres per hour, the first time lithium has ever been seen being produced by a nova.…”

Section: Introductionmentioning

confidence: 99%

A detailed study of lithium in 107 CHEPS dwarf stars

Pavlenko

Jenkins

Ivanyuk

et al. 2018

A&A

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Context. We report results from lithium abundance determinations using high resolution spectral analysis of the 107 metal-rich stars from the Calan-Hertfordshire Extrasolar Planet Search programme. Aims. We aim to set out to understand the lithium distribution of the population of stars taken from this survey. Methods. The lithium abundance taking account of non-local thermodynamical equilibrium effects was determined from the fits to the Li I 6708 Å resonance doublet profiles in the observed spectra. Results. We find that a) fast rotators tend to have higher lithium abundances; b) log N(Li) is higher in more massive and hot stars; c) log N(Li) is higher in stars of lower log g; d) stars with the metallicities >0.25 dex do not show the lithium lines in their spectra; e) most of our planet hosts rotate slower; and f) a lower limit of lithium isotopic ratio is 7 Li/ 6 Li > 10 in the atmospheres of two stars with planets (SWP) and two non-SWP stars. Conclusions. Measurable lithium abundances were found in the atmospheres of 45 stars located at distances of 20−170 pc from the Sun, for the other 62 stars the upper limits of log N(Li) were computed. We found well defined dependences of lithium abundances on T eff , V sin i, and less pronounced for the log g. In case of V sin i we see two sequences of stars: with measurable lithium and with the upper limit of log N(Li). About 10% of our targets are known to host planets. Only two SWP have notable lithium abundances, so we found a lower proportion of stars with detectable Li among known planet hosts than among stars without planets. However, given the small sample size of our planet-host sample, our analysis does not show any statistically significant differences in the lithium abundance between SWP and stars without known planets.

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Early Optical Spectra of Nova V1369 Cen Show the Presence of Lithium

Cited by 102 publications

References 44 publications

Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova

TheGaia-ESO Survey: Sodium and aluminium abundances in giants and dwarfs

A detailed study of lithium in 107 CHEPS dwarf stars

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