The astrophysical environment of the solar birthplace

Our Sun, like all stars, formed within a cold molecular cloud. Astronomical observations and theory provide considerable detail into this process. Yet cosmochemical observations of short-lived radionuclides in primitive meteorites, in particular ⁶⁰Fe, provide unequivocal evidence that the early solar system inherited fresh nucleosynthetic material from the core of a hot, massive star, almost certainly ejected in a supernova explosion. I give a short introduction to the fields of star formation and meteoritics and discuss how the reconciliation of their disparate clues to our origin places strong constraints on the environment of the solar birthplace. Direct injection of supernova ejecta into a protoplanetary disc or a dense molecular core is unlikely since their small sizes require placement unusually close to the massive star. Lower density molecular cloud clumps can capture more ejecta but the radionuclides decay during the slow gravitational collapse. The most likely scenario is on the largest scales via the formation of enriched molecular clouds at the intersection of colliding supernova bubbles in spiral arms.     

Les premières étoiles

The oldest stars of the Galaxy are quite different from common stars, like our Sun. Understanding why it is so, requires to open the question in a cosmological perspective. After the Big Bang, and for at least 300 000 years, the Universe was nearly uniform, and had a very simple chemical composition formed during the hot phase of the Big Bang: only hydrogen, helium and traces of other light elements, deuterium, ³ He, and ⁷ Li. This composition is known as “primordial”. At a later time, about one or two billion years after the Big Bang, condensations developped at all scales, the smallest ones being stars. The most massive stars, reaching very high temperatures at their center, transformed their initial composition by thermonuclear reactions, producing all common elements observed in the solar system, carbon, nitrogen, oxygen, etc. These elements were dispersed into the interstellar medium by mass-ejection at the final stage of evolution of these massive stars, and recycled by subsequent generations of stars. The first stars must have been formed with the primordial composition, whereas later generations had an increasing proportion of elements produced by stellar nucleosynthesis. Intensive searches of stars with no, or very little elements produced by stellar nucleosynthesis have been performed during the last 20 years. Actually more than 100 stars were discovered with a very low proportion of such elements, one thousandth of the proportion in the Sun (in which they amount to about 1.7% by mass), or less. But no star was found with less that 1/10,000 of the solar proportion. So no “primordial” star has been observed yet. The reason why is still an open question.     

2012年,参宿四会爆炸吗?

恒星是宇宙的基本组成单元,中小质量的恒星(如太阳)占绝大部分.中小质量的恒星演化到最后,外壳被损失掉,成为漂亮的行星状星云,而恒星的核则成为白矮星.大质量恒星演化到最后会发生超新星爆炸,产生巨大的能量,留下一个中子星或黑洞.参宿四是一颗大质量恒星,种种迹象表明,它将发生超新星爆炸,但在2012年爆炸的可能性微乎其微,天上不会出现两个"太阳",也不会对地球上人们的生活产生实质性的影响.     

Dark matter bodies in star and planet structures

The lowest frequency of the dipole f mode (surface gravity wave) of the Sun and some other stars is shown to be close to the orbital frequency of a trial body near the star surface, as well as the wave amplitude is shown to be resonantly increased to the values large enough to be observed. Therefore the Sun is considered to be a sensitive detector for hypothetical compact cosmic bodies made of dark matter particles. In this connection some possible characteristics of the dark matter bodies (DMB) are discussed, and DMB orbits in the Sun are calculated within a standard solar model in order to compare the wave amplitudes with data for the solar surface oscillations, and to estimate the masses and radii of the DMB. As well, some possible phenomena in star and planet structures are discussed with special attention on generation of flares of high X-ray classes, specific behavior of the Moon dust, formation of short-time vertical flows in deserts, oceans, and atmospheres on the Earth and other planets.     

Constraints on the kinetic energy of type-Ic supernova explosion from young PSR J1906+0746 in a double neutron star candidate

So far among the nineteen pairs of detected double neutron star (DNS) systems, it is a usual fact that the first-born recycled pulsar is detected, however the youngest DNS system PSR J1906+0746, with the characteristic age of 113 kyr, is one of the three detected DNS as a non-recycled and second-born NS, which is believed to be formed by an electron capture or a low energy ultra-stripped iron core-collapse supernova (SN) explosion. The SN remnant around PSR J1906+0746 is too dim to be observed by optical telescopes, then its x-ray flux limit has been given by Chandra. A reference pulsar PSR J1509-5850 with the young characteristic age of 154 kyr was chosen as an object of comparison, which has an SN remnant observed by Chandra and is believed to be formed by iron core SN explosion. We impose a restriction on the maximum kinetic energy of electron-capture (EC) SN explosion that induces the formation of PSR J1906+0746. The estimated result is (4-8)×10⁵⁰ erg (1 erg=10^-7 J), which is consistent with that of the published simulations of the EC process, i.e., a lower value than that of the conventional iron core SN explosion of (1-2)×10⁵¹ erg. As suggested, EC process for NS formation is pertained to the subluminous type Ic SN by the helium star with ONeMg core, thus for the first time we derived the kinetic energy of EC SN explosion of DNS, which may be reconciled with the recent observation of type Ic SN 2014ft with kinetic energy of 2×10⁵⁰ erg.     

太阳日冕物质抛射的磁流体力学性质

太阳是离地球最近的一颗恒星，太阳日冕物质抛射是太阳大气中最剧烈的一种活动现象．当日冕物质抛射爆发时，大量的等离子体物质从接近太阳日面的低日冕被抛出，瞬时释放出巨大的能量．当一部分这些物质和能量传播到地球附近时，可以造成短波通讯中断、卫星工作失常等破坏性现象．文章作者认为，是缠绕的太阳磁场提供了足够的能量，使这些日冕物质可以克服恒星的重力以及周边磁场的束缚抛射出来；而磁螺度在日冕中的不断积累，不仅为日冕物质抛射提供了能量基础，而且使爆发在一定程度上成为一种日冕演化的必然。     

超子耦合参数对热前中子星物质的影响

在相对论平均场理论框架内,利用Λ超子的结合能和中子星质量的观测数据得到超子标量介子耦合参数χσ的范围是0.33—0.77。在这个范围内, 研究了χσ取不同值时, 包含核子, Λ和Ξ超子的热前中子星（固定单个重子熵s=1）的性质。结果表明, 如果超子耦合参数变大, 前中子星核心温度变高, 中微子丰度变低, 前中子星的亚稳态质量范围变小。如果χσ超过了0.75, 前中子星不可能演变成黑洞。联系SN1987A讨论了这一结果的意义。In the framework of the relativistic mean field theory(RMFT), protoneutron stars with hyperons are studied. To be compatible with neutron star masses, the hyperon scalar coupling χσ should lie in the range of 0.33—0.77. As the hyperon scalar coupling increases, in protoneutron star matter, the core temperature increases whereas the abundance of neutrinos decreases. The metastable mass range of protoneutron stars narrows as the temperature increases. It is found that a protoneutron star cannot subside into a low mass black hole when χσ>0.75. Furthermore, the case of SN1987A is discussed.     

太阳系的元素丰度分布与AGB星慢中子俘获元素

通过对AGB星演化模型的理论计算结果和51颗AGB星的观测丰度进行重新分析,发现任何AGB星与慢中子俘获过程(s过程)主要分量对应的重元素(简称SMH元素)丰度分布都与对应的太阳系s过程主要分量的元素丰度分布相似,这表明,任意AGB星SMH元素丰度分布的迭加结果与对应的太阳系s过程主要分量的元素丰度分布相似,由此得出结论:太阳系s过程主要分量的重元素丰度分布模式是一个典型的模式,可以作为标准用于单星重元素丰度的研究.     

Constraining the neutrino magnetic moment with antineutrinos from the sun

We discuss the impact of different solar neutrino data on the spin-flavor-precession (SFP) mechanism of neutrino conversion. We find that, although detailed solar rates and spectra allow the SFP solution as a subleading effect, the recent KamLAND constraint on the solar antineutrino flux places stronger constraints on this mechanism. Moreover, we show that for the case of random magnetic fields inside the Sun, one obtains a more stringent constraint on the neutrino magnetic moment down to the level of mu(nu)< or = few x 10(-12)mu(B), similar to bounds obtained from star cooling.     

Transient solar oscillations driven by primordial black holes

Stars are transparent to the passage of primordial black holes (PBHs) and serve as seismic detectors for such objects. The gravitational field of a PBH squeezes a star and causes it to ring acoustically. We calculate the seismic signature of a PBH passing through the Sun. The background for this signal is the observed spectrum of solar oscillations excited by supersonic turbulence. We predict that PBHs more massive than 10(21) g (comparable in mass to an asteroid) are detectable by existing solar observatories. The oscillations excited by PBHs peak at large scales and high frequencies, making them potentially detectable in other stars. The discovery of PBHs would have profound implications for cosmology and high-energy physics.     

A pulsar inside the Sun?

The Crimean observation of solar oscillations in 1974–1982 showed that the basic period of pulsation of the Sun hidden in its deep interior was equal to P ₀=160.0101±0.0001min. More recently, the period was changed to the new value P ₁=159.9662±0.0006min, which almost coincided with the annual sidelobe of the former period P ₀. The amplitude of the P₁ oscillation has increased considerably over 1994–1995. We substantiate the hypothesis that a) the change in the period was caused by the interaction of the P₀ oscillation with the rapid rotation of the solar core and that b) the latter has the form of a compact, highly magnetized object like a neutron star rotating with sidereal period P₁.Translated from Izvestiya Vysshikh Uchebnykh Zavedenii, Radiofizika, Vol. 39, No. 10, pp. 1210–1214, October, 1996.The author expresses his gratitude to the referee for his honest and useful comments to this paper. The author is also thankful to V. I. Haneychuk and T. T. Tsap for their active participation in the solar observations at the CrAO which were used in the present paper. This work was supported in part by the International Science Foundation under Grants No. UCU000 and UCU200.     

A black hole preying on the star for a gamma-ray burst of GRB080503: Evidence for the second event in this new class

In this paper, we critically assess GRB080503, a short gamma-ray burst with very bright extended emission (about 30 times the gamma-ray fluence of the initial spike). The light curve of the prompt γ-ray emission of GRB080503 resembles that of GRB 060614 which has been suggested to be due to an event from an intermediate mass black hole (IMBH) preying on a star. We therefore propose that GRB080503 is also due to a similar event; the mass of the IMBH is estimated to be about 4.6×10⁴ solar masses, and the engulfed star had about the same mass and size as the Sun. We also estimate that the total burst energy is about 7.67 × 10⁵⁰ ergs.

     

How to use the Sun–Earth Lagrange points for fundamental physics and navigation

We illustrate the proposal, nicknamed LAGRANGE, to use spacecraft, located at the Sun–Earth Lagrange points, as a physical reference frame. Performing time of flight measurements of electromagnetic signals traveling on closed paths between the points, we show that it would be possible: (a) to refine gravitational time delay knowledge due both to the Sun and the Earth; (b) to detect the gravito-magnetic frame dragging of the Sun, so deducing information about the interior of the star; (c) to check the possible existence of a galactic gravitomagnetic field, which would imply a revision of the properties of a dark matter halo; (d) to set up a relativistic positioning and navigation system at the scale of the inner solar system. The paper presents estimated values for the relevant quantities and discusses the feasibility of the project analyzing the behavior of the space devices close to the Lagrange points.     

Strangeness in stellar matter

A protoneutron star is formed immediately after the gravitational collapse of the core of a massive star. At birth, the hot and high density matter in such a star contains a large number of neutrinos trapped during collapse. Trapped neutrinos generally inhibit the presence of exotic matter — hyperons, a kaon condensate, or quarks. However, as the neutrinos diffuse out in about 10–15 s, the threshold for the appearance of strangeness is reduced; hence, the composition and the structure of the star can change significantly. The effect of exotic, negatively-charged, strangeness-bearing components is always to soften the equation of state, and the possibility exists that the star collapses to a black hole at this time. This could explain why no neutron star has yet been seen in the remnant of supernova SN1987A, even though one certainly existed when neutrinos were detected on Feb. 23, 1987. With new generation neutrino detectors it is feasible to test different theoretical scenarios observationally.     

May a supernova bang twice?

The Mont Blanc group reports a burst of neutrinos in the LSD detector occuring the day before the optical discovery of SN1987A. The Kamiokande (K2) and IMB experiments see neutrino bursts ∼4 h 43 min after LSD. The K2 observations at LSD time here said to contradict LSD. I argue that the K2 results strongly support the LSD pulse(!). I critically analyse the data, and prove that all experiments are compatible at all times. I discuss the plausibility and predictive power of a two-neutrino-burst scenario, wherein the progenitor's core first became a neutron star, and subsequently recollapsed into a black hole (or strange star) as matter left behind by a partially failed shock wave accreted on and around the neutron star, with a calculated fall-back time of a few hours     

The meridional circulation of the Sun: Observations,theory and connections with the solar dynamo

The meridional circulation of the Sun, which is observed to be poleward at the surface, should have a return flow at some depth. Since large-scale flows like the differential rotation and the meridional circulation are driven by turbulent stresses in the convection zone, these flows are expected to remain confined within this zone. Current observational(based on helioseismology)and theoretical(based on dynamo theory) evidences point towards an equatorward return flow of the meridional circulation at the bottom of the convection zone. Assuming the mean values of various quantities averaged over turbulence to be axisymmetric,we study the large-scale flows in solar-like stars on the basis of a 2D mean field theory. Turbulent stresses in a rotating star can transport angular momentum, setting up a differential rotation. The meridional circulation arises from a slight imbalance between two terms which try to drive it in opposite directions: a thermal wind term(arising out of the higher efficiency of convective heat transport in the polar regions) and a centrifugal term(arising out of the differential rotation). To make these terms comparable,the poles of the Sun should be slightly hotter than the equator. We discuss the important role played by the meridional circulation in the flux transport dynamo model. The poloidal field generated by the Babcock-Leighton process at the surface is advected poleward, whereas the toroidal field produced at the bottom of the convection zone is advected equatorward. The fluctuations in the meridional circulation(with coherence time of about 30-40 yr) help in explaining many aspects of the irregularities in the solar cycle. Finally, we discuss how the Lorentz force of the dynamo-generated magnetic field can cause periodic variations in the large-scale flows with the solar cycle.     

The need to measure low-energy antineutrinos (<Emphasis Type="Italic">E</Emphasis><Subscript><Emphasis Type="Italic">⊻</Emphasis></Subscript><0.782 MeV) from the Sun

Measurements are needed of low-energy antineutrinos generated by possible neutron decay at the core of the Sun. The measurement will test the validity of a proposal that solar luminosity, solar neutrinos, and the outpouring of H⁺ ions from the solar surface are the products of a chain of reactions triggered by neutron emission from the solar core. Inverse β decay of 87-d ³⁵S, induced by capture of low-energy antineutrinos on ³⁵Cl, is a likely candidate for this measurement.     

Quark matter in astrophysics and cosmology

We discuss the role of quark matter in astrophysics and cosmology. The implications of the dynamics of the quark-hadron phase transition in the early universe for the element abundances from big gang nucleosynthesis and the composition of the dark matter in the universe are addressed. We discuss the possibility of deciding on an equation of state for high density matter by observing the cooling of a neutron star remnant of SN1987A. Quark matter models for the Centauros events, Cygnus X-3 cosmic ray events, high energy gamma-ray bursts and the solar neutrino problem are described.     

How to see an antistar

Polarization of photons emitted in weak decays occurring at distant star makes it possible to determine whether this star is made from antimatter. The observation of neutrinos (antineutrinos) produced at neutronization (antineutronization) reactions at the beginning of SN $\left( {\overline {SN} } \right)$ explosion is even more promising.     

Explosion mechanism of collapse-driven supernovae

Recent theoretical development of collapse-driven supernova explosion is reviewed. In particular, we discuss in detail i) convection in the hot bubble region above the protoneutron star as the source of the large amplitude velocity fluctuations which is necessary to explain large scale mixing in SN1987 A, and ii) jet-like explosion induced by axisymmetric neutrino emission from a rotating oblate proto-neutron star, which might account for asymmetry of expanding envelope of SN1987 A.