The origin of lithium (Li) and its production process have long been uncertain. Li could be produced by Big Bang nucleosynthesis, interactions of energetic cosmic rays with interstellar matter, evolved low-mass stars, novae, and supernova explosions. Chemical evolution models and observed stellar Li abundances suggest that at least half the Li may have been produced in red giants, asymptotic giant branch (AGB) stars, and novae1,2,3. No direct evidence, however, for the supply of Li from evolved stellar objects to the Galactic medium has hitherto been found. Here we report the detection of highly blue-shifted resonance lines of the singly ionized radioactive isotope of beryllium, 7Be, in the near-ultraviolet spectra of the classical nova V339 Del (Nova Delphini 2013) 38 to 48 days after the explosion. 7Be decays to form 7Li within a short time (half-life of 53.22 days4). The 7Be was created during the nova explosion via the alpha-capture reaction 3He(α,γ)7Be (ref. 5). This result supports the theoretical prediction that a significant amount of 7Li is produced in classical nova explosions.
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Romano, D., Matteucci, F., Molaro, P. & Bonifacio, P. The galactic lithium evolution revisited. Astron. Astrophys. 352, 117–128 (1999)
Romano, D., Matteucci, F., Ventura, P. & D'Antona, F. The stellar origin of 7Li. Do AGB stars contribute a substantial fraction of the local Galactic lithium abundance? Astron. Astrophys. 374, 646–655 (2001)
Prantzos, N. Production and evolution of Li, Be, and B isotopes in the Galaxy. Astron. Astrophys. 542, A67 (2012)
Audi, G., Bersillon, O., Blachot, J. & Wapstra, A. H. The NUBASE evaluation of nuclear and decay properties. Nucl. Phys. A 729, 3–128 (2003)
Cameron, A. G. W. & Fowler, W. A. Lithium and the s-PROCESS in Red-Giant Stars. Astrophys. J. 164, 111–114 (1971)
Waagen, E. O. Nova Delphini 2013 = PNV J20233073+2046041. AAVSO Alert Notice 489, (2013)
Munari, U. et al. After a post-maximum plateau Nova Del 2013 has begun a normal decline. Astron. Telegr. 5304, 1 (2013)
Williams, R., Mason, E., Della Valle, M. & Ederoclite, A. Transient heavy element absorption systems in novae: episodic mass ejection from the secondary star. Astrophys. J. 685, 451–462 (2008)
Sadakane, K., Tajitsu, A., Mizoguchi, S., Arai, A. & Naito, H. Discovery of multiple high-velocity narrow circumstellar NaI D lines in Nova V1280 Sco. Publ. Astron. Soc. Jpn 62, L5–L10 (2010)
McLaughlin, D. B. in Stellar Atmospheres (ed. Greenstein, J. L. ) 585–652 (The University of Chicago Press, 1960)
Skopal, A. et al. Early evolution of the extraordinary Nova Delphini 2013 (V339 Del). Astron. Astrophys. 569, A112 (2014)
Williams, R. E. The formation of novae spectra. Astron. J. 104, 725–733 (1992)
Warner, B. Cataclysmic variable stars. Camb. Astrophys. Ser. 28, 257–306 (1995)
Kramida, A., Ralchenko, Yu., Reader, J. & the NIST ASD team. NIST Atomic Spectra Database Ver. 5.1 http://physics.nist.gov/asd (National Institute of Standards and Technology, 2013)
Yan, Z.-C., Nörtershäuser, W. & Drake, G. W. F. High precision atomic theory for Li and Be+: QED shifts and isotope shifts. Phys. Rev. Lett. 100, 243002 (2008)
Arnould, M. & Norgaard, H. The explosive thermonuclear formation of 7Li and 11B. Astron. Astrophys. 42, 55–70 (1975)
Starrfield, S., Truran, J. W., Sparks, W. M. & Arnould, M. On Li-7 production in nova explosions. Astrophys. J. 222, 600–603 (1978)
D'Antona, F. & Matteucci, F. Galactic evolution of lithium. Astron. Astrophys. 248, 62–71 (1991)
Boffin, H. M. J., Paulus, G., Arnould, M. & Mowlavi, N. The explosive thermonuclear formation of Li-7 revisited. Astron. Astrophys. 279, 173–178 (1993)
Hernanz, M., Jose, J., Coc, A. & Isern, J. On the synthesis of 7Li and 7Be in novae. Astrophys. J. 465, L27–L30 (1996)
José, J. & Hernanz, M. Nucleosynthesis in classical novae: CO versus ONe white dwarfs. Astrophys. J. 494, 680–690 (1998)
Naito, H., Tajitsu, A., Arai, A. & Sadakane, K. Discovery of metastable helium absorption lines in V1280 Scorpii. Publ. Astron. Soc. Jpn 65, 37 (2013)
Harris, M. J. et al. Transient gamma-ray spectrometer observations of gamma-ray lines from novae. III. The 478 keV line from 7Be decay. Astrophys. J. 563, 950–957 (2001)
Hernanz, M. in Classical Novae (eds Bode, M. F. & Evans, A. ) 2nd edn, 252–284 (Cambridge Astrophys. Ser. 43, Cambridge University Press, 2008)
Sackmann, I.-J. & Boothroyd, A. I. Creation of 7Li and destruction of 3He, 9Be, 10B, and 11B in low-mass red giants, due to deep circulation. Astrophys. J. 510, 217–231 (1999)
de la Reza, R., da Silva, L., Drake, N. A. & Terra, M. A. On 7Li enrichment by low-mass metal-poor red giant branch stars. Astrophys. J. 535, L115–L117 (2000)
Sackmann, I.-J. & Boothroyd, A. I. The creation of superrich lithium giants. Astrophys. J. 392, L71–L74 (1992)
Travaglio, C. et al. Galactic chemical evolution of lithium: interplay between stellar sources. Astrophys. J. 559, 909–924 (2001)
Ventura, P. & D'Antona, F. The role of lithium production in massive AGB and super-AGB stars for the understanding of multiple populations in globular clusters. Mon. Not. R. Astron. Soc. 402, L72–L76 (2010)
Melo, C. H. F. et al. On the nature of lithium-rich giant stars. Constraints from beryllium abundances. Astron. Astrophys. 439, 227–235 (2005)
Munari, U. & Henden, A. Photometry of the progenitor of Nova Del 2013 (V339 Del) and calibration of a deep BVRI photometric comparison sequence. Inform. Bull. Variable Stars 6087, 1 (2013)
Deacon, N. R. et al. Pre-outburst observations of Nova Del 2013 from Pan-STARRS 1. Astron. Astrophys. 563, A129 (2014)
Denisenko, D. et al. V339 Delphini = Nova Delphini 2013 = Pnv J20233073+2046041. IAU Circ. No. 9258, 2 (2013)
The Fermi-LAT Collaboration. Fermi establishes classical novae as a distinct class of gamma-ray sources. Science 345, 554–558 (2014)
Schaefer, G. H. et al. The expanding fireball of Nova Delphini 2013. Nature 515, 234–236 (2014)
Noguchi, K. et al. High Dispersion Spectrograph (HDS) for the Subaru Telescope. Publ. Astron. Soc. Jpn 54, 855–864 (2002)
Shenavrin, V. I., Taranova, O. G. & Tatarnikov, A. M. Dust formation in Nova Del 2013. Astron. Telegr. 5431, 1 (2013)
Tajitsu, A., Aoki, W., Kawanomoto, S. & Narita, N. Nonlinearity in the detector used in the Subaru Telescope High Dispersion Spectrograph. Publ. Natl. Astron. Obs. Jpn 13, 1–8 (2010)
Massey, P., Strobel, K., Barnes, J. V. & Anderson, E. Spectrophotometric standards. Astrophys. J. 328, 315–333 (1988)
Moore, C. E. A Multiplet Table of Astrophysical Interest: NBS Technical Note No. 36, Reprinted Version of the 1945 edition (US Department of Commerce, 1959)
Kurucz, R. & Bell, B. Atomic Line Data CD-ROM No. 23 (Smithsonian Astrophysical Observatory, 1995)
This work is based on data collected at the Subaru Telescope, which is operated by the National Astronomical Observatory of Japan (NAOJ). We acknowledge with thanks the variable star observations from the AAVSO International Database contributed by observers worldwide and used in this research.
The authors declare no competing financial interests.
Extended data figures and tables
V (green) and R (red) magnitudes are taken from the AAVSO database. The epochs of our HDS observations are indicated by arrows.
a, The radial velocity plots of three Fe ii emission lines belonging to the same multiplet number30 (42). In addition to the similarity of their broad emission profiles, all lines have common blue-shifted absorption line features around vrad ≈ −1,000 km s−1. b, An enlarged view of the absorption line features in a. Dips of individual absorption line are indicated with dashed lines. c, The absorption line systems in H i Balmer lines drawn on the same velocity scale as in b.
a, The overall view of the spectrum from 308 nm to 350 nm. Identified Fe ii emission lines are indicated with red ticks at the bottom. The identified absorption line systems originating from iron-group ions are indicated by coloured ticks at the top: Fe ii (red), Ti ii (blue), Cr ii (green), Mn ii, Ni ii, and V ii (black). b, A sample of the absorption line identification. The results of our identification are displayed along the spectrum. c, As for Extended Data Fig. 2b, but for two lines (Ti ii and Cr ii), highlighted in b, which are plotted on the velocity scale.
a–c, The horizontal scale is displayed with the heliocentric (bottom) and the Doppler-corrected wavelengths (top). The Doppler corrections are applied using vdays = v+38, v+47, and v+48 for panels a, b, and c, respectively. The local continuums, fitted with high-order (10–20) spline functions, are overplotted with green lines. The positions of the strongest (vrad = vdays) and the second-strongest components of the absorption line system are indicated by coloured long and short lines connected by horizontal bars. d, Since no apparent absorption lines are found in day +52, a Doppler correction using v+48 is applied to the spectrum.
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Tajitsu, A., Sadakane, K., Naito, H. et al. Explosive lithium production in the classical nova V339 Del (Nova Delphini 2013). Nature 518, 381–384 (2015) doi:10.1038/nature14161
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