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首页> 外文期刊>Nature >Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger
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Spectroscopic identification of r-process nucleosynthesis in a double neutron-star merger

机译：双中子星合并中r-过程核合成的光谱鉴定

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摘要

The merger of two neutron stars is predicted to give rise to three major detectable phenomena: a short burst of gamma-rays, a gravitational-wave signal, and a transient optical-near-infrared source powered by the synthesis of large amounts of very heavy elements via rapid neutron capture (the r-process)(1-3). Such transients, named 'macronovae' or 'kilonovae'(4-7), are believed to be centres of production of rare elements such as gold and platinum(8). The most compelling evidence so far for a kilonova was a very faint near-infrared rebrightening in the afterglow of a short gamma-ray burst(9,10) at redshift z = 0.356, although findings indicating bluer events have been reported(11). Here we report the spectral identification and describe the physical properties of a bright kilonova associated with the gravitational-wave source(12) GW170817 and gamma-ray burst(13,14) GRB 170817A associated with a galaxy at a distance of 40 megaparsecs from Earth. Using a series of spectra from ground-based observatories covering the wavelength range from the ultraviolet to the near-infrared, we find that the kilonova is characterized by rapidly expanding ejecta with spectral features similar to those predicted by current models(15,16). The ejecta is optically thick early on, with a velocity of about 0.2 times light speed, and reaches a radius of about 50 astronomical units in only 1.5 days. As the ejecta expands, broad absorption-like lines appear on the spectral continuum, indicating atomic species produced by nucleosynthesis that occurs in the post-merger fast-moving dynamical ejecta and in two slower (0.05 times light speed) wind regions. Comparison with spectral models suggests that the merger ejected 0.03 to 0.05 solar masses of material, including high-opacity lanthanides.
机译：预计两个中子星的合并将引起三个主要的可检测现象：伽马射线的短脉冲，引力波信号以及由大量非常重的合成驱动的瞬态光学近红外源元素通过快速中子捕获（r过程）（1-3）。这样的瞬变被称为“宏新星”或“基洛诺娃”（4-7），被认为是稀有元素（如金和铂）的生产中心（8）。迄今为止，最令人信服的证据是，在红移z = 0.356时，短伽玛射线爆发（9,10）的余辉中产生了非常微弱的近红外再增亮，尽管据报道发现发现了更蓝的事件（11）。在这里我们报告光谱识别并描述与引力波源（12）GW170817和与银河系相距40兆帕秒距离的伽玛射线爆发（13,14）GRB 170817A相关的明亮的新星的物理特性。利用来自地面观测站的一系列光谱，涵盖了从紫外线到近红外的波长范围，我们发现千伏新星的特征是快速扩张的射流，其光谱特征与当前模型预测的相似（15,16）。弹射体很早就具有光学厚度，其速度约为光速的0.2倍，仅1.5天就达到了约50个天文单位的半径。随着射流的扩展，在光谱的连续谱上会出现宽的吸收样线，表明核合成产生的原子种类出现在合并后快速移动的动力射流和两个较慢的风速（光速的0.05倍）中。与光谱模型的比较表明合并产生了0.03至0.05太阳质量的材料，包括高不透明镧系元素。

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  • 来源
    《Nature》 |2017年第7678期|67-70|共4页
  • 作者

    Pian E.; DAvanzo P.; Enetti S. B.; Ranchesi M. B.; Rocato E. B.; Campana S.; Cappellaro E.; Covino S.; DElia V.; Fynbo J. P. U.; Getman F.; Ghirlanda G.; Ghisellini G.; Grado A.; Greco G.; Hjorth J.; Kouveliotou C.; Levan A.; Limatola L.; Alesani D. M.; Azzali P. A. M.; Elandri A. M.; Oller P. M.; Icastro L. N.; Palazzi E.; Piranomonte S.; Rossi A.; Salafia O. S.; Selsing J.; Stratta G.; Tanaka M.; Tanvir N. R.; Tomasella L.; Watson D.; Yang S.; Amati L.; Antonelli L. A.; Ascenzi S.; Ernardini M. G. B.; Boer M.; Ufano F. B.; Ulgarelli A. B.; Capaccioli M.; Casella P.; Castro-Tirado A. J.; Chassande-Mottin E.; Ciolfi R.; Copperwheat C. M.; Dadina M.; De Cesare G.; Di Paola A.; Fan Y. Z.; Gendre B.; Giuffrida G.; Giunta A.; Hunt L. K.; Israel G. L.; Jin Z. -P.; Kasliwal M. M.; Klose S.; Lisi M.; Longo F.; Aiorano E. M.; Apelli M. M.; Asetti N. M.; Ava L. N.; Patricelli B.; Perley D.; Pescalli A.; Piran T.; Possenti A.; Pulone L.; Azzano M. R.; Salvaterra R.; Schipani P.; Spera M.; Stamerra A.; Stella L.; Tagliaferri G.; Testa V.; Troja E.; Turatto M.; Ergani S. D. V.; Ergani D. V.;

  • 作者单位

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy|Gran Sasso Sci Inst, Viale F Crispi 7, Laquila, Italy|INFN, Lab Nazl Gran Sasso, I-67100 Laquila, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy|ASI, Space Sci Data Ctr, Via Politecn, I-00133 Rome, Italy;

    Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark;

    INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy;

    Univ Urbino Carlo Bo, Dipartimento Sci Pure & Applicate, Piazza Repubbl 13, I-61029 Urbino, Italy|INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy;

    Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark;

    George Washington Univ, APSIS, Corcoran Hall, Washington, DC 20052 USA|George Washington Univ, Dept Phys, Corcoran Hall, Washington, DC 20052 USA;

    Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England;

    INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy;

    Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark;

    Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,IC2,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England|Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85748 Garching, Germany;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy|Univ Milano Bicocca, Dipartimento Fis G Occhialini, Piazza Sci 3, I-20126 Milan, Italy;

    Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark;

    Univ Urbino Carlo Bo, Dipartimento Sci Pure & Applicate, Piazza Repubbl 13, I-61029 Urbino, Italy|INFN, Sez Firenze, I-50019 Sesto Fiorentino, Italy;

    Natl Astron Observ Japan, Mitaka, Tokyo, Japan;

    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England;

    Univ Copenhagen, Niels Bohr Inst, Dark Cosmol Ctr, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark;

    Padova Univ, Dept Astron & Phys, Padua, Italy|Univ Calif Davis, Dept Astron, Davis, CA 95616 USA;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy|Univ Roma La Sapienza, Dipartimento Fis, Piazzale Aldo Moro 2, I-00185 Rome, Italy|Univ Roma Tor Vergata, Via Ric Sci 1, I-00133 Rome, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy|Univ Montpellier, CNRS IN2P3, Lab Univers & Particules Montpellier, Montpellier, France;

    CNRS, OCA, UCA, ARTEMIS, Blvd Observ,CS 34229, F-06304 Nice 4, France;

    INAF Osservatorio Astron Catania, Via S Sofia 78, I-95123 Catania, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy|Univ Naples Federico II, Dept Phys, Corso Umberto I 40, I-80138 Naples, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    Inst Astrofis Andalucia CSIC, Glorieta Astron, E-18008 Granada, Spain;

    Univ Paris Diderot, APC, CNRS IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite, Paris, France;

    INFN TIFPA, Trento Inst Fundamental Phys & Applicat, Via Sommar 14, I-38123 Trento, Italy;

    Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,IC2,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy|INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China;

    Univ Virgin Isl, 2 John Brewers Bay, St Thomas, VI 00802 USA;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF Osservatorio Astrofis Arcetri, Largo Enrico Fermi 5, I-50125 Florence, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    Chinese Acad Sci, Purple Mt Observ, Key Lab Dark Matter & Space Astron, Nanjing 210008, Jiangsu, Peoples R China;

    CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA;

    Thuringer Landessternwarte Tautenburg, Sternwarte 5, D-07778 Tautenburg, Germany;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    Univ Trieste, I-34127 Trieste, Italy|INFN Trieste, I-34127 Trieste, Italy;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

    Univ Innsbruck, Inst Astrophys & Particle Phys, Technikerstr 25-8, A-6020 Innsbruck, Austria;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy|Univ Andres Bello, Dept Ciencias Fis, Fernandez Concha 700, Santiago, Chile;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy|INAF, Osservatorio Astron Trieste, Via GB Tiepolo 11, I-34143 Trieste, Italy;

    Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy;

    Liverpool John Moores Univ, Astrophys Res Inst, Liverpool Sci Pk,IC2,146 Brownlow Hill, Liverpool L3 5RF, Merseyside, England;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy|Univ Insubria, Via Valleggio 11, I-22100 Como, Italy;

    Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel;

    INAF, Osservatorio Astron Cagliari, Via Sci 5, I-09047 Selargius, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy;

    INAF, Ist Astrofis Spaziale & Fis Cosm Milano, Via E Bassini 15, I-20133 Milan, Italy;

    INAF, Osservatorio Astron Capodimonte, Salita Moiariello 16, I-80131 Naples, Italy;

    Scuola Normale Super Pisa, Piazza Cavalieri 7, I-56126 Pisa, Italy|INAF, Osservatorio Astron Torino, Pino Torinese, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy;

    INAF, Osservatorio Astron Roma, Via Frascati 33, I-00078 Monte Porzio Catone, Italy;

    NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA;

    INAF, Osservatorio Astron Brera, Via E Bianchi 46, I-23807 Merate, Italy|PSL Res Univ, CNRS, Observ Paris, GEPI, Pl Jules Janssen, F-92190 Meudon, France;

    INAF, Inst Space Astrophys & Cosm Phys, Via Gobetti 101, I-40129 Bologna, Italy;

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