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Possible climates on terrestrial exoplanets
Possible climates on terrestrial exoplanets

Full PDF - Royal Society Publishing
Full PDF - Royal Society Publishing

Introduction
Introduction

... which stars die depends on their original mass. In low and intermediate mass stars (∼18 M ) death is preceded by the so-called planetary nebula phase. Our Sun will become a Planetary Nebula in some 5 billion years. Because by far most stars have masses below 8 M , the planetary nebula phase must b ...
Exoplanets - Polarisation.eu
Exoplanets - Polarisation.eu

Pretty Pictures of the Cosmos
Pretty Pictures of the Cosmos

... with the Hubble Space Telescope, distant galaxies form a dramatic backdrop for disrupted spiral galaxy Arp 188, the Tadpole Galaxy. The cosmic Tadpole is a mere 420 million light-years distant toward the northern constellation Draco. Its eye-catching tail is about 280 thousand light-years long and f ...
SIMULATIONS
SIMULATIONS

... Detailed analysis of parameter space from literature gives consistent results ...
Twitter Feed ITSO Symposium 2017
Twitter Feed ITSO Symposium 2017

... galactic inflow/outflow, in understanding the factors affecting galaxy evolution. Disentangling the effect of internal (stellar mass) and external (environment) processes on the galaxy evolution is difficult because high mass galaxies tend to exist in dense environments. For the past decade, the dif ...
Flagship imaging SAG report
Flagship imaging SAG report

Progenitor neutron stars of the lightest and heaviest millisecond
Progenitor neutron stars of the lightest and heaviest millisecond

... stage, 18 M has been ejected from the binary. Frictional dissipation of kinetic energy causes the binary to shrink and shortens its orbital period to ∼4 d. D: Supernova (SN) The outcome of SNIb/c determines the initial state for the IMXB/LMXB evolution stages (Tauris et al. 2011; Lin et al. 2011). ...
Does gravity conserve angular momentum
Does gravity conserve angular momentum

... One of the most remarkable contributions of Oleg Jefimenko is that he developed gravitomagnetism while taking into account the distances between the source and the receptor by taking into account the retardation of the fields by the speed of light [2]. His theory is strictly based upon Oliver Heavis ...
stars - acpsd
stars - acpsd

... The ejection of stellar remnants is the low-mass star�supernova. On Earth, we measure the effects of this supernova in the increased luminosity. After a low-mass star�death (supernova), it often leaves behind material that forms new stellar bodies. This is the end of stars with low masses (less than ...
HD 147506b: A SUPERMASSIVE PLANET IN AN ECCENTRIC
HD 147506b: A SUPERMASSIVE PLANET IN AN ECCENTRIC

Likely formation of general relativistic radiation pressure supported
Likely formation of general relativistic radiation pressure supported

... of Led . As if, a leaking and contracting balloon stops contraction as its self gravity fixes the leakage by forcing the molecules to move in (almost) closed circular orbits. Also, simultaneously, the attendant heat and pressure become large enough to resist further contraction. In a very strict sen ...
Type I SuperNova
Type I SuperNova

... of carbon in a white dwarf. In looking at the spectra of the supernova remnants, very little hydrogen spectra is observed. This might or might not make sense, because the white dwarf has little hydrogen to begin with, but the companion star has hydrogen. ...
Galactic Archaeology: Current Surveys
Galactic Archaeology: Current Surveys

The fate of black hole singularities and the parameters of the
The fate of black hole singularities and the parameters of the

... beginning with an initial value p∗ and letting the system evolve through N generations. Let us define a function B(p) on P that is the expected number of future singularities generated during a lifetime of a universe with parameters5 p. We may observe that, for most p, B(p) is one, but there are sma ...
Chapter 1 Introduction
Chapter 1 Introduction

... Supernovae and supernova remnants ...
MAIN SEQUENCE STARS, Red Giants and White Dwarfs
MAIN SEQUENCE STARS, Red Giants and White Dwarfs

... Dead Core Evolution • They are not massive enough to compress the C core to T > 7 x 108 K at which it could fuse, so these CSPN's just cool off and fade in power, slowly shrinking in size • BUT, when density of the core reaches 106 g/cm3 (or one ton / teaspoon!) the PAULI EXCLUSION PRINCIPLE takes ...
Post-Main Sequence Evolution – Low and Intermediate Mass Stars
Post-Main Sequence Evolution – Low and Intermediate Mass Stars

RXTE PCA Contributions to Monitoring Fast Transients
RXTE PCA Contributions to Monitoring Fast Transients

... Perhaps interaction with the pulsar and the magnetosphere are involved. Other instabilities besides the thermal-viscous disk instability may cause the flips between quiescence and steady accretion. Several sources have had variable accretion in the range 10 34-1035 ergs s-1 for years, while others h ...
ET: Astronomy 230 Outline Important Caveat
ET: Astronomy 230 Outline Important Caveat

The Formation of Population III Stars in Gas Accretion Stage: Effects
The Formation of Population III Stars in Gas Accretion Stage: Effects

... in the region of n ∼ 1017 − 1018 cm−3 , where the circumstellar disk is expected to form. Thus, the magnetic field can dissipate in this region in a primordial cloud. In addition, the magnetic Reynolds number derived in equation (6) is not applicable, especially in the gas accretion phase after first ...
A Human-Powered Orrery - Astronomical Society of the Pacific
A Human-Powered Orrery - Astronomical Society of the Pacific

... generally come up are: 1) how “off ” are the planets due to the assumption of circular orbits (generally about the size of one of the circles or less) and 2), since it is assumed that the planet years are an even multiple of 16 days (8 for Mercury), how long is it before you have to correct for this ...
THE RADIOMETRIC BODE`S LAW AND EXTRASOLAR PLANETS
THE RADIOMETRIC BODE`S LAW AND EXTRASOLAR PLANETS

... fly-bys of the gas giants, as well as measurements of the Earth’s radio emission. In particular, Farrell et al. (1999) considered two forms of the radiometric Bode’s law, one incorporating measurements of only Jupiter and Saturn and the other incorporating all five magnetic planets. The former gives ...
s-process
s-process

... Heavy metals at [Fe/H] = -4 ...
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Nebular hypothesis

The nebular hypothesis is the most widely accepted model in the field of cosmogony to explain the formation and evolution of the Solar System. It suggests that the Solar System formed from nebulous material. The theory was developed by Immanuel Kant and published in his Universal Natural History and Theory of the Heaven. Originally applied to our own Solar System, this process of planetary system formation is now thought to be at work throughout the universe. The widely accepted modern variant of the nebular hypothesis is the solar nebular disk model (SNDM) or simply solar nebular model. This nebular hypothesis offered explanations for a variety of properties of the Solar System, including the nearly circular and coplanar orbits of the planets, and their motion in the same direction as the Sun's rotation. Some elements of the nebular hypothesis are echoed in modern theories of planetary formation, but most elements have been superseded.According to the nebular hypothesis, stars form in massive and dense clouds of molecular hydrogen—giant molecular clouds (GMC). These clouds are gravitationally unstable, and matter coalesces within them to smaller denser clumps, which then rotate, collapse, and form stars. Star formation is a complex process, which always produces a gaseous protoplanetary disk around the young star. This may give birth to planets in certain circumstances, which are not well known. Thus the formation of planetary systems is thought to be a natural result of star formation. A Sun-like star usually takes approximately 1 million years to form, with the protoplanetary disk evolving into a planetary system over the next 10-100 million years.The protoplanetary disk is an accretion disk that feeds the central star. Initially very hot, the disk later cools in what is known as the T tauri star stage; here, formation of small dust grains made of rocks and ice is possible. The grains eventually may coagulate into kilometer-sized planetesimals. If the disk is massive enough, the runaway accretions begin, resulting in the rapid—100,000 to 300,000 years—formation of Moon- to Mars-sized planetary embryos. Near the star, the planetary embryos go through a stage of violent mergers, producing a few terrestrial planets. The last stage takes approximately 100 million to a billion years.The formation of giant planets is a more complicated process. It is thought to occur beyond the so-called frost line, where planetary embryos mainly are made of various types of ice. As a result, they are several times more massive than in the inner part of the protoplanetary disk. What follows after the embryo formation is not completely clear. Some embryos appear to continue to grow and eventually reach 5–10 Earth masses—the threshold value, which is necessary to begin accretion of the hydrogen–helium gas from the disk. The accumulation of gas by the core is initially a slow process, which continues for several million years, but after the forming protoplanet reaches about 30 Earth masses (M⊕) it accelerates and proceeds in a runaway manner. Jupiter- and Saturn-like planets are thought to accumulate the bulk of their mass during only 10,000 years. The accretion stops when the gas is exhausted. The formed planets can migrate over long distances during or after their formation. Ice giants such as Uranus and Neptune are thought to be failed cores, which formed too late when the disk had almost disappeared.
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