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Gas Mass Fractions and the Evolution of Spiral Galaxies
Gas Mass Fractions and the Evolution of Spiral Galaxies

... luminosity and surface brightness. It is not correlated with linear size. Gas fraction varies with luminosity and surface brightness at the same rate, indicating evolution at fixed size. Dim galaxies are clearly less evolved than bright ones, having consumed only ∼ 1/2 of their gas. This resolves th ...
Spectroscopy: Unlocking the Secrets of Star Light
Spectroscopy: Unlocking the Secrets of Star Light

... The slit on the spectrograph limits the light entering the spectrograph so that it acts as a point source of light from a larger image. This allows an astronomer to take a number of spectra from different regions of an extended source such as a galaxy or of s specific star in the telescope's field o ...
Spectroscopy: Unlocking the Secrets of Star Light
Spectroscopy: Unlocking the Secrets of Star Light

... The slit on the spectrograph limits the light entering the spectrograph so that it acts as a point source of light from a larger image. This allows an astronomer to take a number of spectra from different regions of an extended source such as a galaxy or of s specific star in the telescope's field o ...
Constraining the star formation histories of spiral bulges
Constraining the star formation histories of spiral bulges

... Unless otherwise stated, data reduction was carried out using the figaro package of Starlink software. A bias level from the overscan region was subtracted from each frame. Due to the presence of localized features in the flat-field frames, each object was divided by the normalized, average flat-fie ...
Abstract book
Abstract book

... environments. In particular, the spatial distribution of recently formed stars in clusters is an important source of information on the physical conditions of the original gas cloud and on the early dynamical evolution of the cluster stars (see Parker et al. last works). In this context, one of the ...
PPT presentation
PPT presentation

... (2002) presented STIS slitless spectra of the 29 LMC PNe, while Stanghellini et al. (2003) presented STIS images and slitless spectra for 27 SMC PNe. ...
A Spectroscopically Confirmed Excess of 24 micron Sources in a
A Spectroscopically Confirmed Excess of 24 micron Sources in a

... the physics at work. Simulations are sufficiently advanced that new insight can be obtained by, e.g. comparing star formation and gas-loss rates as a function of local density to the observations (Tonnesen et al. 2007). Also, instead of focusing on massive clusters, the key to understanding the inte ...
Elliptical Galaxies
Elliptical Galaxies

... galactic systems comprising just a single component, relatively bright in the center but fading rapidly with increasing radius. Elliptical galaxies are found mostly in the denser regions of the universe, from rich clusters to small groups; truely isolated ellipticals being relatively rare. Figure 1 ...
the chandra deep field–north survey. xvii. evolution of
the chandra deep field–north survey. xvii. evolution of

Lecture26_Future
Lecture26_Future

a changing cosmos - Whittier Union High School District
a changing cosmos - Whittier Union High School District

... has been the name of the nebula ever since. The Crab Nebula, or M1 in Charles Messier’s catalog of “comet impostors,” is in the exact same spot as the recorded position of the “guest star” of 1054. But it wasn’t until 1928 that Edwin Hubble measured the rate of expansion of the Crab nebula which le ...
Science drivers for GLAO at LBT
Science drivers for GLAO at LBT

Planetary Nebulae: Observational Properties, Mimics, and Diagnostics
Planetary Nebulae: Observational Properties, Mimics, and Diagnostics

... 60 kms−1 though some strongly bipolar PN can have considerably higher expansion velocities (up to 300 kms−1 ) along the major axis. By definition, a PN surrounds a hot, low-mass CS, which may in fact be off-centre in some old examples due to an asymmetric ISM interaction (see Wareing 2010, and Sabin ...
Neon abundances - UCL Astrophysics Group
Neon abundances - UCL Astrophysics Group

... Explorer (IUE) on the ultraviolet resonance lines of iron-peak elements in 26 HgMn, four superficially normal and 10 normal stars. We observed definite detections or determined upper limits for Ne i in 21 of the HgMn stars in the Smith & Dworetsky (1993) sample, and in 11 of the normal and superfici ...
The Young Stars
The Young Stars

... named after the prototype discovered in the constellation of Taurus. They displayed erratic optical variability, strong chromospheric lines and could be identified through their strong Hα emission lines. They were found to congregate at the periphery of dark clouds. The nearest were located in the T ...
Binary mass ratios: system mass not primary mass
Binary mass ratios: system mass not primary mass

... stars at the same time. It is worth considering the mass ratio distribution of companions to massive stars. In a model with a universal flat mass ratio distribution B- and O-stars will have a mass ratio distribution tending to low-mass companions very similar to that of A-stars (for the same reason) ...
Stellar evolution – Part III of III - Inside Mines
Stellar evolution – Part III of III - Inside Mines

... • Magnetic fields • Dust disks around the stars Note: the Sun may form a planetary nebula, but uncertain (M☉ too small?) ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
Fluorine abundances in dwarf stars of the solar neighbourhood⋆

... of F/O exclude AGB synthesis as the dominant source of fluorine in their targeted stellar populations. In particular, the targeted stars in ω Cen did not have enhanced F abundances, despite their large s-process abundance values. In addition, they claimed a qualitative agreement with what is expecte ...
Physics 1114OL - Normandale Community College
Physics 1114OL - Normandale Community College

... Recommended: Depending on where you purchased your textbook, there may be a copy of Starry Night packaged with Universe. (Used books may not have the software intact and the college bookstore is not responsible for missing software in used books.) Starry Night is an excellent program and I encourage ...
Gaia talk
Gaia talk

... 100Tb raw compressed data – our database is 15Tb as of today 2 telescopes, 35m focal length, rectangular mirrors 3.5M hours of work to study, design & build = 300people x 7 years 400 scientists working on data processing Over 30,000 mission documents in archive Launch burned 225tonnes of kerosene+ox ...
The star-forming content of the W3 giant molecular cloud
The star-forming content of the W3 giant molecular cloud

... that it does not assume any a priori source profile and that it is an objective technique. Its weaknesses are mainly those associated with the separation of crowded objects and the inclusion of spurious sources at low levels, which are common to all object-detection routines. clfind defines a clump ...
Radial Velocity - Yale Exoplanet
Radial Velocity - Yale Exoplanet

... stars, since the Doppler signal increases as 1/ m1 at ...
Conference Abstract Booklet here.
Conference Abstract Booklet here.

... and OGLE team Blazhko effect is a long-term quasi-periodic amplitude and/or phase modulation of pulsations of RR Lyrae stars. After its discovery in 1907 by Sergey Blazhko, its origin remains a mystery. This phenomenon has not been extensively studied in firstovertone (RRc) RR Lyrae stars yet. The O ...
Lecture Outline and Specific Objectives
Lecture Outline and Specific Objectives

... This outline summarises lecture-by-lecture the main concepts which we hope will be conveyed in Astronomy and which will be regarded as examinable. The order is as currently expected, but may change slightly, or may slip slightly, as lecturers present the material and availability of guest lecturers ...
Emission from dust in galaxies: Metallicity dependence
Emission from dust in galaxies: Metallicity dependence

... region (Osterbrock 1989). Thus, during the resonant scatterings in an H ii region, all the Lyα photons are assumed to be absorbed by grains in IHK00, which this paper is based on. If the dust-to-gas ratio is significantly smaller than the Galactic value, the dust grains might not efficiently absorb ...
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Future of an expanding universe

Observations suggest that the expansion of the universe will continue forever. If so, the universe will cool as it expands, eventually becoming too cold to sustain life. For this reason, this future scenario is popularly called the Big Freeze.If dark energy—represented by the cosmological constant, a constant energy density filling space homogeneously, or scalar fields, such as quintessence or moduli, dynamic quantities whose energy density can vary in time and space—accelerates the expansion of the universe, then the space between clusters of galaxies will grow at an increasing rate. Redshift will stretch ancient, incoming photons (even gamma rays) to undetectably long wavelengths and low energies. Stars are expected to form normally for 1012 to 1014 (1–100 trillion) years, but eventually the supply of gas needed for star formation will be exhausted. And as existing stars run out of fuel and cease to shine, the universe will slowly and inexorably grow darker, one star at a time. According to theories that predict proton decay, the stellar remnants left behind will disappear, leaving behind only black holes, which themselves eventually disappear as they emit Hawking radiation. Ultimately, if the universe reaches a state in which the temperature approaches a uniform value, no further work will be possible, resulting in a final heat death of the universe.
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