Beryllium detection in the very fast nova ASASSN-16kt (V407 Lupi)

Izzo, L.; Molaro, P.; Bonifacio, P.; Valle, M. Della; Cano, Z.; Postigo, A. de Ugarte; Prieto, J. L.; Thöne, C. C.; Vanzi, L.; Zapata, A.; Fernandez, D.

doi:10.1093/mnras/sty435

Cited by 33 publications

(42 citation statements)

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“…(Jose 2016). Our results and those of V5668 Sgr by Molaro et al (2016) and and V407 Lup by Izzo et al (2018) indicate that indeed ONe novae produce less 7 Be than CO novae (although in larger amounts than models).…”

Section: Discussionsupporting

confidence: 72%

“…We note that 7 Be has been positively detected so far in slow novae only, see Tajitsu et al (2016); Molaro et al (2016). However, Izzo et al (2018) detected 7 Be also in the fast ONe V407 Lup. Therefore, these last observations, summarized in Table 6, indicate that synthesis of 7 Be may take place both in slow and in very fast novae, and that ONe novae are also candidate sites.…”

Section: Discussionmentioning

confidence: 94%

“…However, modeling of the outburst of V838 Her (Downen et al 2013;Champagne et al 2014) indicated a massive (1.34-1.35 M ) ONe WD, without com- Tajitsu et al (2015Tajitsu et al ( , 2016 are corrected here for the decay of 7 Be. References are: (1) Tajitsu et al (2015); (2) Molaro et al (2016), (3) Izzo et al (2018) and (4) pelling evidence for breakout (T peak in the TNR close to 3 × 10 8 K). It should be also noted that the hydrodynamic models of Politano et al (1995) and José & Hernanz (1998) predict a sharp reduction of oxygen and significant increase of sulphur as the WD mass increases, although, as pointed out by Schwarz et al (2007), in the case of V838 Her both models fail to produce the observed mass fraction of sulphur.…”

Section: Discussionmentioning

confidence: 99%

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Absorption and emission features of 7Be ii in the outburst spectra of V838 Her (Nova Her 1991)

Selvelli

Molaro

Izzo

2018

Monthly Notices of the Royal Astronomical Society

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High and low resolution IUE spectra of V838 Her in the early outburst stages exhibit a strong absorption feature shortward of λ3130. We discuss the nature of this spectral feature and provide convincing evidence that it corresponds to the blue-shifted resonance doublet of singly-ionized 7 Be recently discovered in other novae. During the evolution of the outburst the appearance of an emission feature close to λ3130Å is also identified as 7 Be ii λ3132 because the usual identification as the O iii λ3133.7 Bowen fluorescence line is hardly compatible with both the known oxygen under-abundance in the nova ejecta and the low optical depths in the nebula due to the high outflow velocity. The average 7 Be abundance relative to hydrogen, estimated by four different methods, i.e. the 7 Be ii/Mg ii absorption ratio, and the 7 Be ii/Mg ii, 7 Be ii/He ii 1640 , and 7 Be ii/Hβ emission ratios is N(Be)/N(H) ≈ 2.5 ×10 −5 (by number), i.e. ≈ 1.7 ×10 −4 by mass. This corresponds to an overproduction of 7 Be by about 1 dex in comparison with the theoretical models of massive CO and ONe novae. Since 7 Be all converts into 7 Li, the 7 Be/H abundance implies a 7 Li/H overabundance of about 4 dex over the 7 Li/H meteoritic value and indicates a total ejected mass of 7 Li of ≈ 9.5×10 −10 M . These data are in line with previous observations and indicate that large amounts of 7 Li can be synthesized in a variety of novae, including very fast ONe novae.

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Section: Discussionsupporting

confidence: 72%

Section: Discussionmentioning

confidence: 94%

Section: Discussionmentioning

confidence: 99%

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Absorption and emission features of 7Be ii in the outburst spectra of V838 Her (Nova Her 1991)

Selvelli

Molaro

Izzo

2018

Monthly Notices of the Royal Astronomical Society

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“…Whilst it is not easy to summarise and review all the works that have addressed Li abundances and Galactic Li evolution in the past thirty years, a few recent observational results can be highlighted. In particular, we note that amongst the proposed contributors to the Li enrichment in the Galaxy, asymptotic giant branch (AGB) stars ejecta, red giants, supernovae, cosmic ray spallation, and novae, recent observations of novae have clearly detected the lines 7 Li or 7 Be (which then decays into 7 Li) at the early stages, showing that these systems may represent a dominant source of Li enrichment in the Galaxy (Izzo et al 2015(Izzo et al , 2018Tajitsu et al 2015;Molaro et al 2016). Along similar lines, recent observations of large samples of giants provide some support to the idea that these stars may also contribute to the Galactic Li enrichment (e.g.…”

Section: ); Nevertheless a Major Question Remains Open; Namely Whatmentioning

confidence: 84%

The Gaia-ESO Survey: Galactic evolution of lithium at high metallicity

Randich

Pasquini

Franciosini

et al. 2020

A&A

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Context. Reconstructing the Galactic evolution of lithium (Li) is the main tool used to constrain the source(s) of Li enrichment in the Galaxy. Recent results have suggested a decline in Li at supersolar metallicities, which may indicate reduced production. Aims. We exploit the unique characteristics of the Gaia-ESO Survey open star cluster sample to further investigate this issue and to better constrain the evolution of Li at high metallicity. Methods. We trace the upper envelope of Li abundance versus metallicity evolution using 18 clusters and considering members that should not have suffered any Li depletion. Results. At variance with previous claims, we do not find any evidence of a Li decrease at high metallicity. The most metal-rich clusters in the sample ([Fe/H] = ∼0.3) actually show the highest Li abundances, with A(Li) > 3.4. Our results clearly show that previous findings, which were based on field stars, were affected by selection effects. The metal-rich population in the solar neighbourhood is composed of relatively old and cool stars that have already undergone some Li depletion; hence, their measured Li does not represent the initial interstellar medium abundance, but a lower limit to it.

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“…Moreover, recently we found that oxygen-neon novae also produce a similar quantity of 7 Be, which then yields 7 Li (Izzo et al 2018). In 2016 ASASSN-16kt, a fast nova in Lupus, was discovered (Izzo et al 2016).…”

Section: First Detections Of 7 LI and 7 Be In Classical Novaementioning

confidence: 97%