Massive stars as thermonuclear reactors and their explosions following core collapse

Nuclear reactions transform atomic nuclei inside stars. This is the process of stellar nucleosynthesis. The basic concepts of determining nuclear reaction rates inside stars are reviewed. How stars manage to burn their fuel so slowly most of the time are also considered. Stellar thermonuclear reactions involving protons in hydrostatic burning are discussed first. Then I discuss triple alpha reactions in the helium burning stage. Carbon and oxygen survive in red giant stars because of the nuclear structure of oxygen and neon. Further nuclear burning of carbon, neon, oxygen and silicon in quiescent conditions are discussed next. In the subsequent core-collapse phase, neutronization due to electron capture from the top of the Fermi sea in a degenerate core takes place. The expected signal of neutrinos from a nearby supernova is calculated. The supernova often explodes inside a dense circumstellar medium, which is established due to the progenitor star losing its outermost envelope in a stellar wind or mass transfer in a binary system. The nature of the circumstellar medium and the ejecta of the supernova and their dynamics are revealed by observations in the optical, IR, radio, and X-ray bands, and I discuss some of these observations and their interpretations.Comment: To be published in " Principles and Perspectives in Cosmochemistry" Lecture Notes on Kodai School on Synthesis of Elements in Stars; ed. by Aruna Goswami & Eswar Reddy, Springer Verlag, 2009. Contains 21 figure

Combustion in thermonuclear supernova explosions

Type Ia supernovae are associated with thermonuclear explosions of white dwarf stars. Combustion processes convert material in nuclear reactions and release the energy required to explode the stars. At the same time, they produce the radioactive species that power radiation and give rise to the formation of the observables. Therefore, the physical mechanism of the combustion processes, as reviewed here, is the key to understand these astrophysical events. Theory establishes two distinct modes of propagation for combustion fronts: subsonic deflagrations and supersonic detonations. Both are assumed to play an important role in thermonuclear supernovae. The physical nature and theoretical models of deflagrations and detonations are discussed together with numerical implementations. A particular challenge arises due to the wide range of spatial scales involved in these phenomena. Neither the combustion waves nor their interaction with fluid flow and instabilities can be directly resolved in simulations. Substantial modeling effort is required to consistently capture such effects and the corresponding techniques are discussed in detail. They form the basis of modern multidimensional hydrodynamical simulations of thermonuclear supernova explosions. The problem of deflagration-to-detonation transitions in thermonuclear supernova explosions is briefly mentioned.Comment: Author version of chapter for 'Handbook of Supernovae,' edited by A. Alsabti and P. Murdin, Springer. 24 pages, 4 figure

Explosive Nucleosynthesis: What we learned and what we still do not understand

This review touches on historical aspects, going back to the early days of nuclear astrophysics, initiated by B$^2$FH and Cameron, discusses (i) the required nuclear input from reaction rates and decay properties up to the nuclear equation of state, continues (ii) with the tools to perform nucleosynthesis calculations and (iii) early parametrized nucleosynthesis studies, before (iv) reliable stellar models became available for the late stages of stellar evolution. It passes then through (v) explosive environments from core-collapse supernovae to explosive events in binary systems (including type Ia supernovae and compact binary mergers), and finally (vi) discusses the role of all these nucleosynthesis production sites in the evolution of galaxies. The focus is put on the comparison of early ideas and present, very recent, understanding.Comment: 11 pages, to appear in Springer Proceedings in Physics (Proc. of Intl. Conf. "Nuclei in the Cosmos XV", LNGS Assergi, Italy, June 2018

Neutrino Signatures From Young Neutron Stars

After a successful core collapse supernova (CCSN) explosion, a hot dense proto-neutron star (PNS) is left as a remnant. Over a time of 20 or so seconds, this PNS emits the majority of the neutrinos that come from the CCSN, contracts, and loses most of its lepton number. This is the process by which all neutron stars in our galaxy are likely born. The emitted neutrinos were detected from supernova (SN) 1987A, and they will be detected in much greater numbers from any future galactic CCSN. These detections can provide a direct window into the properties of the dense matter encountered inside neutron stars, and they can affect nucleosynthesis in the material ejected during the CCSN. In this chapter, we review the basic physics of PNS cooling, including the basic equations of PNS structure and neutrino diffusion in dense matter. We then discuss how the nuclear equation of state, neutrino opacities in dense matter, and convection can shape the temporal behavior of the neutrino signal. We also discuss what was learned from the late-time SN 1987A neutrinos, the prospects for detection of these neutrinos from future galactic CCSNe, and the effects these neutrinos can have on nucleosynthesis

PERAN ORANG TUA DALAM MEMBINA NILAI KARAKTER ANAK DI KECAMATAN SIMPANG TIGA ACEH BESAR

ABSTRAKRahmayanti KS, Sri. 2016. Peran Orang Tua Dalam Membina Nilai Karakter Anak di Kecamatan Simpang Tiga Kabupaten Aceh Besar. Skripsi, Jurusan Pendidikan Kesejahteraan Keluarga, Fakultas Keguruan dan Ilmu Pendidikan, Universitas Syiah Kuala. Pembimbing:(1)Dr. Anizar Ahmad, M.Pd., (2). Dra. Fitriana, M.SI.Kata Kunci: Nilai Karakter Anak, Peran Orang TuaPeran orang tua adalah partisipasi atau kesadaran jiwa orang tua untuk memperdulikan anaknya, terutama dalam hal memberikan dan memenuhi kebutuhan hidup anaknya baik dari segi sosial maupun material. Penelitian ini untuk mengetahui usaha orang tua dalam membina nilai karakter anak di Kecamatan Simpang Tiga Kabupaten Aceh Besar. Penelitian ini bertujuan untuk (1) mengetahui usaha yang dilakukan orang tua dalam membina nilai karakter anak dan (2) mengetahui sistem pengawasan yang diterapkan oleh orang tua terhadap anak. Metode yang digunakan dalam penelitian ini adalah metode deskriptif kuantitatif. Data penelitian ini bersumber dari orang tua yang memiliki anak usia 4 sampai 10 tahun berjumlah 28 keluarga, pengumpulan data menggunakan kuisioner. Pengolahan data penelitian ini menggunakan rumus persentase. Simpulan penelitian ini berpengaruh pada usaha orang tua dalam membina nilai karakter anak, walau sebagian kecil yang mengetahui nilai-nilai karakter, tetapi sebagian besar sudah berusaha menanamkan nilai karakter tersebut. Lebih dari setengah responden menanamkan nilai religius kepada anak dengan tujuan agar anak mempunyai akhlak yang mulia kedepannya. Sedangkan yang berperan dalam membina nilai karakter anak adalah suami dan istri. Sistem pengawasan yang diterapkan orang tua berpengaruh terhadap pembentukkan nilai karakter anak. Seluruh anak termasuk kedalam katagori anak yang mudah bersahabat. Penanaman nilai karakter pada anak di mulai pada awal masa kanak-kanak ketika berumur 2-6 tahun. Responden juga menerapkan perilaku disiplin kepada anak karena usia awal kanak-kanak merupakan usia yang masih rentan, dan akan meniru semua yang dikerjakan oleh orang tuanya. Saran untuk orang tua agar dapat mendidik anaknya dengan baik, tidak mengedepankan emosi, dapat meluangkan waktu, adanya komunikasi yang dibina orang tua dengan anak, dan jangan bersikap apatis terhadap apa yang dikerjakan sianak

Taming trilogues: the EU's law-making process in a comparative perspective.

Trilogues have become the modus operandi of EU decision-making. They are an informal but institutionalised mechanism providing for in camera discussions of legislative texts between the three main EU decision-making institutions, with a view to securing legislative compromises. Trilogues present risks to an organ of parliamentary representation through their potential to depoliticise conflict and by reducing the accountability and transparency of the decision-making process. We examine how the European Parliament (EP) has responded to trilogues and what this response tells us about the development of the EP as an institutionalised organ of representative democracy. We compare these with arrangements for bicameral conflict resolution in the United States, where similar issues are presented by informal mechanisms of decision-making. We assess the institutionalisation of trilogues from a democratic perspective, highlighting achievements and future challenges, and the value of these findings for the ongoing reflection on the EP as a normal parliament and the role of informal institutions in EU law-making

Implications for Post-processing Nucleosynthesis of Core-collapse Supernova Models with Lagrangian Particles

We investigate core-collapse supernova (CCSN) nucleosynthesis with self-consistent, axisymmetric (2D) simulations performed using the neutrino hydrodynamics code Chimera. Computational costs have traditionally constrained the evolution of the nuclear composition within multidimensional CCSN models to, at best, a 14-species α-network capable of tracking only (α, γ)reactions from 4He to 60Zn. Such a simplified network limits the ability to accurately evolve detailed composition and neutronization or calculate the nuclear energy generation rate. Lagrangian tracer particles are commonly used to extend the nuclear network evolution by incorporating more realistic networks into post-processing nucleosynthesis calculations. However, limitations such as poor spatial resolution of the tracer particles; inconsistent thermodynamic evolution, including misestimation of expansion timescales; and uncertain determination of the multidimensional mass cut at the end of the simulation impose uncertainties inherent to this approach. We present a detailed analysis of the impact of such uncertainties for four self-consistent axisymmetric CCSN models initiated from solar-metallicity, nonrotating progenitors of 12, 15, 20, and 25 and evolved with the smaller α-network to more than 1 s after the launch of an explosion

Implications for Post-processing Nucleosynthesis of Core-collapse Supernova Models with Lagrangian Particles

We investigate core-collapse supernova (CCSN) nucleosynthesis with self-consistent, axisymmetric (2D) simulations performed using the neutrino hydrodynamics code Chimera. Computational costs have traditionally constrained the evolution of the nuclear composition within multidimensional CCSN models to, at best, a 14-species α-network capable of tracking only (α, γ)reactions from 4He to 60Zn. Such a simplified network limits the ability to accurately evolve detailed composition and neutronization or calculate the nuclear energy generation rate. Lagrangian tracer particles are commonly used to extend the nuclear network evolution by incorporating more realistic networks into post-processing nucleosynthesis calculations. However, limitations such as poor spatial resolution of the tracer particles; inconsistent thermodynamic evolution, including misestimation of expansion timescales; and uncertain determination of the multidimensional mass cut at the end of the simulation impose uncertainties inherent to this approach. We present a detailed analysis of the impact of such uncertainties for four self-consistent axisymmetric CCSN models initiated from solar-metallicity, nonrotating progenitors of 12, 15, 20, and 25 and evolved with the smaller α-network to more than 1 s after the launch of an explosion