论文标题
魅力对新生儿磁铁的超基因中微子的贡献
Charm contribution to ultrahigh-energy neutrinos from newborn magnetars
论文作者
论文摘要
新生儿，强烈磁化的中子星（所谓的磁铁）被其恒星或合并喷射包围的新生儿，预计将通过在质子上加速到超大型能量的质质子中产生的中微子来源，这是通过在质子上加速到超级能量的蛋白质中产生的超高能量中微子的来源。我们表明，不仅是由于其较小的生产横截面而被忽视的不仅是pions和kaons，而且还可以代表超高能量中的中微子液体的主要贡献，因为它们的一生很短，而超高能源中微子的中微子在早期产生了pion和Kaon的生产而受到抑制。我们表明，下一代探测器，例如极端的多理智天体物理学探测器（诗歌），用于Neurtino检测的巨型无线电阵列（Grand）和Icecube-gen2很有可能观察中微子，主要来自Charm Hadrons，来自附近的Magnetars。我们还表明，可以在$ 10^2 $ s到$ 10^3 $ s的时间间隔内观察到来自附近磁铁驱动的Novae的中微子，在该时间间隔中，魅力强体的贡献主要是$ 10^8 $ gev，与下一代探测器相关的中微子能量。我们还评论了魅力强子对弥漫性中微子通量贡献的潜在影响。
Newborn, strongly magnetized neutron stars (so-called magnetars) surrounded by their stellar or merger ejecta are expected to be sources of ultrahigh-energy neutrinos via decay of mesons produced in hadronic interactions of protons which are accelerated to ultrahigh energies by magnetic dissipation of the spindown energy. We show that not only pions and kaons but also charm hadrons, which are typically neglected due to their small production cross sections, can represent dominant contributions to neutrino fluence at ultrahigh energies, because of their short lifetimes, while the ultrahigh-energy neutrino fluence from pion and kaon production is suppressed at early times due to their significant cooling before their decay. We show that the next-generation detectors such as Probe Of Extreme Multi-Messenger Astrophysics (POEMMA), Giant Radio Array for Neurtino Detection (GRAND) and IceCube-Gen2 have a good chance of observing neutrinos, primarily originating from charm hadrons, from nearby magnetars. We also show that neutrinos from nearby magnetar-driven merger novae could be observed in the time interval between $10^2$ s and $10^3$ s, where the charm hadron contribution is dominant for neutrino energies above $10^8$ GeV, of relevance to next generation detectors. We also comment on potential impacts of the charm hadron contribution to the diffuse neutrino flux.
