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Updated
Updated

THE 2MASS WIDE-FIELD T DWARF SEARCH. II. DISCOVERY OF
THE 2MASS WIDE-FIELD T DWARF SEARCH. II. DISCOVERY OF

Local Universe Supernovae and Their Host Galaxies
Local Universe Supernovae and Their Host Galaxies

... Observational properties •NOT homogeneous • show H, He, O, Ca …... • from small to huge radio and X-ray emission Interpretation: The core collapse in massive • occur only (!!) stars in spiral (M≥8Mgalaxies endare of aassociated series central ) at theand with star forming nuclear regions burnings w ...
The XMM-Newton Bright Serendipitous Survey
The XMM-Newton Bright Serendipitous Survey

... sources is relatively easy given the combination of the good positions of the XMM-Newton sources (90% error ∼400 , Della Ceca et al. 2004) and the brightness of the sources: X-ray sources with FX >10−13 erg cm−2 s−1 are expected to have an optical counterpart brighter than 22 mag for X-ray-to-optica ...
Discovery and Study of Exotic Radio Pulsars Jason William Thomas
Discovery and Study of Exotic Radio Pulsars Jason William Thomas

Binary and Millisecond Pulsars | SpringerLink
Binary and Millisecond Pulsars | SpringerLink

... neutron star’s emission beam. Profile stability is of key importance in pulsar timing measurements discussed in Section 4. The selection of integrated profiles in Figure 4 shows a rich diversity in morphology including two examples of “interpulses” – a secondary pulse separated by about 180 degrees ...
the fixed stars
the fixed stars

STARLAB
STARLAB

relative age difference between the metal
relative age difference between the metal

... (2002 April and 2003 May) as the observations of the GC M92 (NGC 6341) reported by Cho and Lee using the same instrumental setup. The data for M53 is reduced using the same method as used for M92 by Cho and Lee, including preprocessing, point-spread function fitting photometry, and standardization e ...
The VIMOS Ultra-Deep Survey (VUDS): Fast Increase in the Fraction
The VIMOS Ultra-Deep Survey (VUDS): Fast Increase in the Fraction

https://tel.archives-ouvertes.fr/file/index/docid/1058049/filename/HOU_XIAN_2013.pdf
https://tel.archives-ouvertes.fr/file/index/docid/1058049/filename/HOU_XIAN_2013.pdf

... This is a milestone in my life, even though there is still definitely a long way to go in the ultimate pursuit of science. I owe my deep acknowledgements to all who have made me who I am today. First of all, I’m extremely grateful to David Smith, my thesis supervisor, for having accepted me to be a ...
The effect of stellar limb darkening values on the accuracy of the
The effect of stellar limb darkening values on the accuracy of the

... Some modellers fix the limb darkening coefficients according to these or other tables when they fit a transit curve. As is clear from the aforementioned discrepancies, in some temperature regions this is not a good strategy because the values of the limb darkening coefficients are not consistent and ...
CONSTRUCTING A PYTHON PIPELINE FOR ANALYZING
CONSTRUCTING A PYTHON PIPELINE FOR ANALYZING

The Observer`s Guide to the Gamma-Ray Burst
The Observer`s Guide to the Gamma-Ray Burst

... being roughly 15,000 to 20,000 km s−1 more rapid than the other GRB-SNe. SN 2013ez is also a notable outlier due to its low line velocity (4000 − 6000 km s−1 ), and inspection of its spectrum (Fig. 5) reveals fewer broad features than other GRB-SNe, where it more closely resembles type Ic SNe rather ...
Document
Document

... • T Tau Sa - A ~3 Solar mass star • Though it is optically invisible, T Tau Sa is the most massive star in the T Tau system! • It is ~50% more massive than T Tau N (one of the brightest & most massive YSOs in Taurus!) • How can this be? ...
A SUB-SATURN MASS PLANET ORBITING HD 36511 Debra A
A SUB-SATURN MASS PLANET ORBITING HD 36511 Debra A

... determined with the spectral synthesis technique described by Butler et al. (1996). Individual observations at Lick Observatory (particularly from the CAT) have photon-limited errors with a signalto-noise ratio of less than 100, so two or three consecutive CAT observations are usually obtained, and ...
Particle Physics from Stars
Particle Physics from Stars

The empirical grounds of SN
The empirical grounds of SN

... a) we may be seeing intrinsically similar phenomena under different angles. GRB 030329/SN 2003dh may be viewed ~ pole-on, GRB 980425/SN 1998bw considerably off-axis (15-30°, Maeda et al. 2005). GRB 031203/SN 2003lw may lie in between (Ramirez-Ruiz et al. 2005) In this scenario the g-properties are ...
c Copyright by Jonathan C. McKinney, 2004
c Copyright by Jonathan C. McKinney, 2004

CoRoT III programme
CoRoT III programme

ASTE Simultaneous HCN(4–3) and HCO+(4–3)
ASTE Simultaneous HCN(4–3) and HCO+(4–3)

... Luminous infrared galaxies (LIRGs) are the population which radiates the bulk of their large luminosities (L & 1011 L¯ ) as infrared dust emission (Sanders & Mirabel 1996). Their large infrared luminosities mean that: (1) powerful energy sources are present, hidden behind dust; (2) energetic radiati ...
365 days of SKYWATCHING
365 days of SKYWATCHING

... the Moon’s orbit will either carr y it nor th or south of the Ear th’s shadow, but about ever y six months it will slip inside that shadow and a lunar eclipse will occur. When it passes only par tially into the cone of shadow it is known as a penumbral eclipse and when it is directly aligned it will ...
Galaxy morphology, luminosity, and environment in the SDSS DR7
Galaxy morphology, luminosity, and environment in the SDSS DR7

... and blue) using data from the Sloan Digital Sky Survey (SDSS), correcting the luminosities for the intrinsic absorption. We use the global luminosity density field to define different environments, and analyse the environmental dependence of galaxy morphology and colour. The smoothed bootstrap method ...
The white dwarf luminosity function
The white dwarf luminosity function

Revising the census of low luminosity AGN
Revising the census of low luminosity AGN

... ONLY A FEW PERCENT! MOST OF THEM HAVE LOW EW AND ARE UNLIKELY TO BE AGN THE LINE EMISSION IS PRODUCED BY THE HOST GALAXY, NOT BY THE AGN THE LINERs REGION IS MOSTLY POPULATED BY NON-AGN THE EW IS A BEST PREDICTOR FOR GENUINE AGN THAN THE DIAGNOSTIC DIAGRAMS A LOW EW (~1 Å) IS CHARACTERISTIC OF STELL ...
1 2 3 4 5 ... 549 >

Star formation



Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.
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