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Topic: Molecular cloud

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Cosmology

	Dark nebula - Wikipedia, the free encyclopedia (Site not responding. Last check: 2007-11-07)
		Molecular clouds consist mainly of gas and dust but contain many stars as well.
		The cloud cores are completely hidden from view and would be undetectable except for the microwave emissions from their constituent molecules.
		The material within the clouds is clumped together in all sizes, with some clouds ranging down to the masses of individual stars, small clumps may extend about one light-year across.
	en.wikipedia.org /wiki/Giant_Molecular_Cloud (415 words)

	The Milky Way in Molecular Clouds (Site not responding. Last check: 2007-11-07)
		These clouds, the location of essentially all star formation, are composed almost entirely of molecular hydrogen and atomic helium, both nearly impossible to detect.
		The intense yellow-to-white horizontal strip at the center of the map is produced by the large number of molecular clouds in the inner spiral arms of the Galaxy, while elsewhere in the map individual nearby molecular clouds are prominent.
		Molecular clouds at higher latitude (and the LMC and M31) are therefore excluded.
	cfa-www.harvard.edu /cfa/hotimage/milky.html (376 words)

	Giant molecular cloud (Site not responding. Last check: 2007-11-07)
		molecular biologia molecular molecular structure molecular motor molecular diabetes molecular biology molecular cell biology plant molecular biology cloud cloud nine radioactive cloud containing saint cloud st.cloud state
		Cloud Descendants of William Cloud and William Harvey as compiled by Ken Cloud of Warner Robins, GA USA.
		John Mitchell Group Research in molecular aggregation, protein ligand-interactions, molecular evolution, prediction of molecular properties, and the molecular basis of odour.
	www.serebella.com /encyclopedia/article-Giant_molecular_cloud.html (335 words)

	Hughes, Self-Similarity in the Rosette Molecular Cloud
		The Rosette Molecular cloud is a star-forming region of gas and dust in the Milky Way which exhibits a highly complex structure with regions of varying density and temperature.
		However, the processes connecting the conditions in a molecular cloud to the observed properties of young stars are not well understood.
		The size-linewidth relation, a well-studied trend in molecular clouds that displays the degree to which the kinematics of the cloud are interconnected on various scales, exhibited a large degree of scatter and a different power law than that generally measured for molecular clouds.
	www.ifa.hawaii.edu /reu/2004research/hughes.html (799 words)

	Star formation - Open Encyclopedia (Site not responding. Last check: 2007-11-07)
		In the current paradigm of star formation, cores of molecular clouds (regions of especially high density) become gravitationally unstable, fragment and begin to collapse.
		The structure of the molecular cloud and the effects of the protostar are best observed in rotational transitions of CO and other molecules; these are observed in the millimeter and submillimeter range.
		The radiation from the protostar and early star has to be observed in infrared astronomy wavelengths, the extinction caused by the rest of the cloud where it is being formed is usually too big to allow us to observe it in the visual part of the spectrum.
	open-encyclopedia.com /Star_formation (403 words)

	Molecular cloud (Site not responding. Last check: 2007-11-07)
		Molecular clouds are interstellar nebulae that have a density and size to permit the formation of H
		Catalogues of clouds exhibit that most the molecular mass is concentrated in the massive object which comprise several million solar They inhabit a plane of roughly 50–75 parsec scale height much thinner than the gaseous components like atomic and ionized hydrogen.
		At the same the clouds are known to be disrupted some process—most likely the effects of massive a significant fraction of their mass has stars.
	www.freeglossary.com /Molecular_cloud (507 words)

	molecular cloud
		It is widely believed that the relatively high density of dust particles in these clouds plays an important role in the formation and protection of the molecules.
		The emission of molecular lines often shows several distinct intensity peaks, each representing individual clumps or clouds of gas and dust in a region that characteristically extends for 50 light-years and is often associated with T Tauri stars —; young, pre-main-sequence stars —; and also hot massive stars and the ionized gas around them.
		Two distinct types, of molecular cloud are known, both associated with star formation: giant molecular clouds and dwarf molecular clouds.
	www.daviddarling.info /encyclopedia/M/molcloud.html (205 words)

	News in Science - Nearby pulsating star cloud puzzles astronomers - 21/03/2003
		Dr Charles Lada of the Harvard Smithsonian Centre for Astrophysics in Boston and colleagues studied the dark molecular cloud known as Barnard 68 and found the signatures of both in-falling and out-flowing material at different locations across the face of the cloud.
		Barnard 68 is a molecular cloud near the constellation Ophiuchus.
		The American astronomers believe that this particular cloud, together with a smattering of others nearby, are the remnants of a much larger cloud that was broken apart by the strong stellar winds and ultraviolet radiation of young and heavy stars as well as supernova explosions in the galactic neighbourhood.
	www.abc.net.au /science/news/stories/s804604.htm (616 words)

	Oort Cloud
		The structure of the cloud is believed to consist of a relatively dense core that lies near the ecliptic plane and gradually replenishes the outer boundaries, creating a steady state.
		One sixth of an estimated six trillion icy objects or comets are in the outer region with the remainder in the relatively dense core.
		The Oort cloud is the source of long-period comets and possibly higher-inclination intermediate comets that were pulled into shorter period orbits by the planets, such as Halley and Swift-Tuttle.
	www.solarviews.com /eng/oort.htm (710 words)

	Cold Diffusion - Page 1
		Molecular clouds are extremely cold nebulae, with temperatures ranging from about -440 to -370 degrees Fahrenheit and consist mostly of hydrogen molecules.
		Molecular clouds have been thought to be stable because of, among other things, the presence of magnetic fields, which, if sufficiently strong, could prevent the molecular clouds from collapsing under their own gravity.
		Stars form when regions of molecular clouds collapse from gravitational instability, as in the case of the young, bright star emerging at the top left edge.
	access.ncsa.uiuc.edu /Stories/mhd (420 words)

	SWAS Science - Primary Targets
		Within these condensations radiation from the many sources in the galaxy is reduced to levels that allows the formation of a rich variety of molecular species, leading astronomers to label the dense regions of the ISM as molecular clouds.
		The differences seen in the spatial distribution of molecular emission within the Orion cloud are quite striking, with the CH emission strongest near the center of the map at the position of an embedded cluster of young stars, while the N
		In addition to being smaller, dark cloud cores do not form as many massive stars as giant cloud cores and therefore are thought to contain more pristine molecular material, material which has not been affected by the formation of stars.
	sao-www.harvard.edu /swas/science3.html (941 words)

	APOD: 2001 September 23 - Molecular Cloud Barnard 68 (Site not responding. Last check: 2007-11-07)
		Here, a high concentration of dust and molecular gas absorb practically all the visible light emitted from background stars.
		molecular clouds some of the coldest and most isolated places in the universe.
		molecular clouds like Barnard 68 form, but it is known that these clouds are themselves likely places for
	antwrp.gsfc.nasa.gov /apod/ap010923.html (150 words)

	molecular cloud - Hutchinson encyclopedia article about molecular cloud (Site not responding. Last check: 2007-11-07)
		In astronomy, enormous cloud of cool interstellar dust and gas containing hydrogen molecules and more complex molecular species.
		Giant molecular clouds (GMCs), about a million times as massive as the Sun and up to 300 light years in diameter, are regions in which stars are being born.
		This information should not be considered complete, up to date, and is not intended to be used in place of a visit, consultation, or advice of a legal, medical, or any other professional.
	encyclopedia.farlex.com /molecular+cloud (116 words)

	Molecular cloud - Wikipedia, the free encyclopedia
		Within a few million years the light from bright stars will have boiled away this molecular cloud of gas and dust.
		The cloud has broken off from the Carina Nebula.
		At the same time, the clouds are known to be disrupted by some process—most likely the effects of massive stars—before a significant fraction of their mass has become stars.
	www.wikipedia.org /wiki/Molecular_cloud (449 words)

	The Birth of Stars
		A high concentration of molecular hydrogen and dust causes the molecular cloud to absorb all light from the stars behind it.
		The centers of such molecular clouds are probably among the coldest places in the Universe.
		Molecular clouds, which are the origination of many stars, are very difficult to study because they are primarily composed of molecular hydrogen at temperatures only about 10 degrees above absolute zero.
	csep10.phys.utk.edu /astr162/lect/birth/birth.html (527 words)

	Spaceflight Now \| Breaking News \| Molecular cloud 300 light-years away has a heartbeat
		Such dense, cold clouds of dust and gas appear fl in photos because the dust blocks visible light from background stars.
		Lada speculates that the shockwave from an exploding star may have smacked into the molecular cloud in the relatively recent past.
		Lada now plans to examine the handful of other molecular clouds that are close enough for high-resolution observations in order to see if any others show signs of pulsation.
	www.spaceflightnow.com /news/n0303/01molecularcloud (1147 words)

	In Search of Planetary Pancakes (Site not responding. Last check: 2007-11-07)
		The problem has to do with molecular clouds, huge gaseous conglomerations of matter — mostly molecular hydrogen (hence the name) along with helium and a trace of other elements.
		Molecular clouds appear to be at least 10 million years old, and maybe 20 to 30 million years."
		Density of the molecular cloud as simulated (increasing from dark blue to red) at one plane through the cubic grid.
	www.psc.edu /science/Norman/in_search_of_planetary_pancakes.html (1579 words)

	Star nurseries: Not much to drink and very hard to breathe
		Because the interstellar clouds are considered to be nurseries for star formation, the SWAS science team is attempting to understand the chemical reactions that affect star birth.
		Both water and molecular oxygen have been considered to be essential constituents of the molecular clouds from which stars form.
		The almost complete absence of molecular oxygen, Goldsmith says, is harder to explain because the molecule doesn't freeze in the same way as water and, thus, would not be in frozen form on dust grains.
	www.eurekalert.org /pub_releases/2001-01/CUNS-SnNm-0901101.php (836 words)

	sciforums.com - Molecular Cloud Barnard 68 (Site not responding. Last check: 2007-11-07)
		What used to be considered a hole in the sky is now known to astronomers as a dark molecular cloud.
		The eerily dark surroundings help make the interiors of molecular clouds some of the coldest and most isolated places in the universe.
		It is not known exactly how molecular clouds like Barnard 68 form, but it is known that these clouds are themselves likely places for new stars to form.
	www.sciforums.com /printthread.php?t=16904 (162 words)

	Stellar evolution (Site not responding. Last check: 2007-11-07)
		One does not study stellar evolution by observing the life cycle of a single star; but rather, by observing numerous stars, each at a different point in its life cycle, and by running computer models which simulate the structure of stars.
		In the beginning, there is the Giant Molecular Cloud.
		A cloud is stable, its constituent molecules too widely spaced for gravity to draw them closer, until a supernova explodes nearby, sending out a shockwave of successive compression and rarefaction analogous to a soundwave travelling through air, forming knots of matter, cores of greater density.
	www.sciencedaily.com /encyclopedia/stellar_evolution (1823 words)

	[No title]
		The star formation areas, known as giant molecular clouds, should be rotating rapidly, spinning up as they collapse like spinning ice skaters drawing in their arms.
		Nearly every giant molecular cloud in M33 within the survey region was detected, and the clouds have sizes and shapes similar to those found in our own galaxy.
		Almost half of the clouds are rotating in a direction opposite to that of the very diffuse gas from which the clouds are produced.
	bima.astro.umd.edu /releases/20020109.html (1061 words)

	The Orion Cloud and Association
		This cloud was formed when a density wave, related to the Galaxy's spiral structure, moved through the medium of the Galactic disk.
		This giant cloud, or complex of clouds, of interstellar matter and young stars contains, besides M42 and M43 and the nebulosity associated with them (NGC 1973-5-7), a number of famous objects: Barnard's Loop, the Horsehead Nebula region (also containing NGC 2024 = Orion B), and the reflection nebulae around M78.
		They must have left the Orion cloud about 2--5 million years ago, and it is speculated that they might have speeded up somehow during supernova explosions (perhaps of companion stars in multiple systems).
	www.seds.org /messier/more/oricloud.html (691 words)

	Report of the Galactic Molecular Clouds and Astrochemistry Working Group
		The major question in Astrochemistry and Molecular Clouds is how molecules and dust grains cycle from the circumstellar envelopes of dying stars through diffuse and dense interstellar clouds, and how they are affected by the formation of new stars.
		The MMA will image with unrivalled clarity galactic molecular clouds to address the most fundamental questions concerning their structure: the nature and origin of the apparent filamentary and turbulent structure, how this dynamic structure evolves into gravitationally bound cores that are destined to form stars, and how the dust properties vary across clouds.
		The Clouds provide unique laboratories for investigating how astrochemistry and molecular cloud structures respond to different conditions of element abundances, stellar populations, external radiation field, mean pressure of the ISM, ambient large-scale gravitational potential, etc., in comparison with the quite different conditions in the Milky Way.
	www.mma.nrao.edu /science/galactic/chem.html (3549 words)

	2MASS
		In addition, a distributed stellar population is inferred in the Orion A and MonR2 molecular clouds within the uncertainties of the field star subtraction with a surface density between 0.013 - 0.083 arcmin**-2.
		The observed mean stellar surface density as a function of Galactic latitude (top panels), the mean residuals after subtracting a polynomial fit to the observed star counts (middle panels), and the RMS of the residuals (bottom panels) at J, H, and Ks band.
		The fraction of the total stellar population currently contained in clusters as a function of the cloud age assuming that only part of the distributed population is detected at a given age as indicated by the model calculations shown in Figure 19.
	www.astro.caltech.edu /~jmc/papers/2mass_clouds (1261 words)

	Astron. Astrophys. 336, 290-300 (1998) (Site not responding. Last check: 2007-11-07)
		A dense molecular cloud is situated adjacent to the eastern border of the clumped continuum emission region.
		The cloud is part of the negative velocity feature, an elongated complex of Galactic center molecular clouds distinguished by its coherent kinematic structure across about a degree in longitude.
		Higher angular resolution data confirm the association between the filaments and a second molecular cloud at a position where the nonthermal filaments are bent, as was previously suggested by Bally and Yusef-Zadeh (1989).
	aa.springer.de /bibs/8336001/2300290/small.htm (332 words)

	Disruption of molecular clouds by ionizing radiation (Site not responding. Last check: 2007-11-07)
		It is not known when and why a region in a molecular cloud commences gravitational collapse to subsequently forms stars.
		Density enhancements in the cloud are excavated due to their higher inertia and could eventually be totally separated from the molecular cloud.
		The isolation of the excavated clumps from the molecular could forms a mechanism for limiting the mass in the envelopes of protostars and young stars.
	www.mpia-hd.mpg.de /THEORY/preprints/kessel/1999/dissertation/node5.html (945 words)

	STAR FORMING REGIONS NEAR THE SUPERNOVA REMNANT IC-443 (Site not responding. Last check: 2007-11-07)
		In the case of W-28, far-infrared observations have shown that a massive, O-type star and possibly a pre-main sequence B-type star are associated with the molecular cloud and its environment.
		In the current study, the northern component of the IC-443 molecular cloud has been detected at 20, 27 and 93-microns by the FIRSSE survey as a far-infrared source.
		The luminosity of this source, assuming a distance of 1.5 kpc, is 130 Lsun, consistent with the expected luminosity of a B7 V star.
	www.astronomycafe.net /anthol/ic443.html (171 words)

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