Summary: Star Formation Near and Far
... an accretion flow, but more work is needed to demonstrate this. What about the possibility of continuing fragmentation? In principle, one could imagine that a collapsing clump might fragment hierarchically into smaller and smaller objects until fragmentation is stopped by the increase of opacity at ...
... an accretion flow, but more work is needed to demonstrate this. What about the possibility of continuing fragmentation? In principle, one could imagine that a collapsing clump might fragment hierarchically into smaller and smaller objects until fragmentation is stopped by the increase of opacity at ...
April 2006 Newsletter PDF - Cowichan Valley Starfinders Society
... elements heavier than hydrogen. This is surprising, says Chapman, because one of the key differences thought to exist between Andromeda and the Milky Way was that the former's stellar halo was metal-rich and the latter's was metal-poor. If both galaxies are metal-poor, then they must have had very s ...
... elements heavier than hydrogen. This is surprising, says Chapman, because one of the key differences thought to exist between Andromeda and the Milky Way was that the former's stellar halo was metal-rich and the latter's was metal-poor. If both galaxies are metal-poor, then they must have had very s ...
13 The Family of Stars
... a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence because this is where most stars are. The white dwarf region is also indicated; these stars are hot but not very luminous because they are qu ...
... a pattern begins to form: These are the 80 closest stars to us; note the dashed lines of constant radius. The darkened curve is called the main sequence because this is where most stars are. The white dwarf region is also indicated; these stars are hot but not very luminous because they are qu ...
Presentation
... • Dense regions in molecular clouds (>one million particles per cm3) • If the cloud is big enough, it will undergo gravitational collapse ...
... • Dense regions in molecular clouds (>one million particles per cm3) • If the cloud is big enough, it will undergo gravitational collapse ...
FOURTH GRADE UNIVERSE - Math/Science Nucleus
... Stars are balls of gas that emit energy created by fusion, a nuclear reaction within the star. There are many sizes and brightness of stars, ranging from super hot, blue-white stars (over 20,000°K) to cool red stars (3,000°K). Our Sun is a medium yellow star, towards the small and cool end of the sp ...
... Stars are balls of gas that emit energy created by fusion, a nuclear reaction within the star. There are many sizes and brightness of stars, ranging from super hot, blue-white stars (over 20,000°K) to cool red stars (3,000°K). Our Sun is a medium yellow star, towards the small and cool end of the sp ...
Galaxies (and stars) in the far infrared: results from the AKARI All
... powerful tool to understand the properties of all classes of objects in the Universe. But first, we need to know: what they are? From our point of view, the crucial point was: which of these sources are the galaxies, how they can be distinguished from sources which belong to Milky Way? If, e.g., we ...
... powerful tool to understand the properties of all classes of objects in the Universe. But first, we need to know: what they are? From our point of view, the crucial point was: which of these sources are the galaxies, how they can be distinguished from sources which belong to Milky Way? If, e.g., we ...
An introduction to the HR diagram File
... stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
... stars are very long lived as they use their fuel so slowly. Very low mass M stars live many billions of years and will simply run out of fuel without dramatic events. ...
Merak
... To the Greeks, this star was named Helike, one of their names to the whole constellation, Ursa Major. According to Burnham, Merak is part of a star cluster including at least 16 other stars from the Ursa Major area of the sky. (http://domeofthesky.com/clicks/merak.html) ...
... To the Greeks, this star was named Helike, one of their names to the whole constellation, Ursa Major. According to Burnham, Merak is part of a star cluster including at least 16 other stars from the Ursa Major area of the sky. (http://domeofthesky.com/clicks/merak.html) ...
Topics for Today`s Class Luminosity Equation The Heart of
... • The Sun is a yellow-white G2 star. • Most stars including the Sun have properties along the mainsequence strip running from hot high-luminosity stars at upper left to cool low-luminosity stars at lower right. Fig. 9-8, p. 179 ...
... • The Sun is a yellow-white G2 star. • Most stars including the Sun have properties along the mainsequence strip running from hot high-luminosity stars at upper left to cool low-luminosity stars at lower right. Fig. 9-8, p. 179 ...
V: 0
... **Teacher will model how to do this** 2. For each star, put an “X” next to the element name for each element it has on RM 21. ...
... **Teacher will model how to do this** 2. For each star, put an “X” next to the element name for each element it has on RM 21. ...
Heavy Metal from Ancient Superstars
... The abundances of the “light” heavy metals in ancient stars are too high to explain with our current theory of supernova r-process production ...
... The abundances of the “light” heavy metals in ancient stars are too high to explain with our current theory of supernova r-process production ...
On the nature of early-type emission line objects in NGC6611
... Intrinsic instellar reddening (E(B-V)) was measured for each star by means of the instellar lines detected at 443.0 and 661.3 nm, and was used to correct the UBVI, JHK (taken from the 2MASS survey), 3.6µm, 4.5µm, 5.7µm and 8µm (SPITZER) magnitudes. Each SED is normalized to the SED of a non ELS clas ...
... Intrinsic instellar reddening (E(B-V)) was measured for each star by means of the instellar lines detected at 443.0 and 661.3 nm, and was used to correct the UBVI, JHK (taken from the 2MASS survey), 3.6µm, 4.5µm, 5.7µm and 8µm (SPITZER) magnitudes. Each SED is normalized to the SED of a non ELS clas ...
Quantum Well Electron Gain Structures and Infrared
... • Venus is MUCH hotter (by about 60K) than we expect • Due to its thick atmosphere and greenhouse gases • So … thick atmosphere can “ruin” a planet in the close end of the HZ • Alternately, it can keep a planet just outside the distant end of the HZ “warm” ...
... • Venus is MUCH hotter (by about 60K) than we expect • Due to its thick atmosphere and greenhouse gases • So … thick atmosphere can “ruin” a planet in the close end of the HZ • Alternately, it can keep a planet just outside the distant end of the HZ “warm” ...
Spectroscopic parallax
... The relationship between a Cepheid variable's luminosity and variability period is quite precise, and has been used as a standard candle (astronomical object that has a know luminosity) for almost a century. This connection was discovered in 1912 by Henrietta Swan Leavitt. She measured the brightnes ...
... The relationship between a Cepheid variable's luminosity and variability period is quite precise, and has been used as a standard candle (astronomical object that has a know luminosity) for almost a century. This connection was discovered in 1912 by Henrietta Swan Leavitt. She measured the brightnes ...
Solutions
... by the newly formed OB Association stars that emit most of their energy as high-energy short-wavelength hardUV photons. The photons from the OB Association stars “power up” the HII region and keep it fluorescing. Thus the OB Association forms first and then the HII region is created around the vicin ...
... by the newly formed OB Association stars that emit most of their energy as high-energy short-wavelength hardUV photons. The photons from the OB Association stars “power up” the HII region and keep it fluorescing. Thus the OB Association forms first and then the HII region is created around the vicin ...
Newfoundland Sky in Summer
... We see the stars only in the night-time, but they are always in the sky. During the day the brighter light of the sun hides the lesser light of the stars, just as a candle would be less noticeable in a brightly lit room than in a dark one. The sun itself i s a star. Other stars are bigger and bright ...
... We see the stars only in the night-time, but they are always in the sky. During the day the brighter light of the sun hides the lesser light of the stars, just as a candle would be less noticeable in a brightly lit room than in a dark one. The sun itself i s a star. Other stars are bigger and bright ...
Stellar populations
... ASTR112 The Galaxy Lecture 3 The cluster turn-off point • This is the (B-V) colour index of bluest mainsequence stars, and corresponds to most massive stars still on M-S (core hydrogen-burning stage). ...
... ASTR112 The Galaxy Lecture 3 The cluster turn-off point • This is the (B-V) colour index of bluest mainsequence stars, and corresponds to most massive stars still on M-S (core hydrogen-burning stage). ...
N5128PNSydney
... Case B). Limit is Schlegel et al. (1998) EBV=0.11 [O III]/Hβ shows no trend, except some higher values near centre (Field 42). Assuming most PN have similar stellar temperature and most of O in O++ => O/H abundance [Ne III]/[O III] very constant as found in other PN studies (MW, MC’s). Ne/O ratio ‘f ...
... Case B). Limit is Schlegel et al. (1998) EBV=0.11 [O III]/Hβ shows no trend, except some higher values near centre (Field 42). Assuming most PN have similar stellar temperature and most of O in O++ => O/H abundance [Ne III]/[O III] very constant as found in other PN studies (MW, MC’s). Ne/O ratio ‘f ...
about Stars
... • Astronomers quantify the “color” of a star by using the difference in brightness between the brightness in the B and V spectral regions • The B-V color is related to the slope of the ...
... • Astronomers quantify the “color” of a star by using the difference in brightness between the brightness in the B and V spectral regions • The B-V color is related to the slope of the ...
Galaxies - Stockton University
... (chemically similar to beach sand) in the galaxy. An emission peak (red) within the bottom of the trough is the chemical signature for molecular hydrogen. The hydrocarbons (orange) are organic molecules comprised of carbon and hydrogen, two of the most common elements on Earth. Since it has taken mo ...
... (chemically similar to beach sand) in the galaxy. An emission peak (red) within the bottom of the trough is the chemical signature for molecular hydrogen. The hydrocarbons (orange) are organic molecules comprised of carbon and hydrogen, two of the most common elements on Earth. Since it has taken mo ...
Lecture 8a Star Formation 10/15/2014
... • Stars are formed from interstellar material which is compressed by gravity • Spend >90% of their lives burning Hydrogen into Helium • How they “die” depends on mass " large stars blow up Supernovas • Understand stars’ lifecycles by studying their properties and also groups of stars ...
... • Stars are formed from interstellar material which is compressed by gravity • Spend >90% of their lives burning Hydrogen into Helium • How they “die” depends on mass " large stars blow up Supernovas • Understand stars’ lifecycles by studying their properties and also groups of stars ...
Serpens
Serpens (""the Serpent"", Greek Ὄφις) is a constellation of the northern hemisphere. One of the 48 constellations listed by the 2nd-century astronomer Ptolemy, it remains one of the 88 modern constellations defined by the International Astronomical Union. It is unique among the modern constellations in being split into two non-contiguous parts, Serpens Caput (Serpent's Head) to the west and Serpens Cauda (Serpent's Tail) to the east. Between these two halves lies the constellation of Ophiuchus, the ""Serpent-Bearer"". In figurative representations, the body of the serpent is represented as passing behind Ophiuchus between Mu Serpentis in Serpens Caput and Nu Serpentis in Serpens Cauda.The brightest star in Serpens is the red giant star Alpha Serpentis, or Unukalhai, in Serpens Caput, with an apparent magnitude of 2.63. Also located in Serpens Caput are the naked-eye globular cluster Messier 5 and the naked-eye variables R Serpentis and Tau4 Serpentis. Notable extragalactic objects include Seyfert's Sextet, one of the densest galaxy clusters known; Arp 220, the prototypical ultraluminous infrared galaxy; and Hoag's Object, the most famous of the very rare class of galaxies known as ring galaxies.Part of the Milky Way's galactic plane passes through Serpens Cauda, which is therefore rich in galactic deep-sky objects, such as the Eagle Nebula (IC 4703) and its associated star cluster Messier 16. The nebula measures 70 light-years by 50 light-years and contains the Pillars of Creation, three dust clouds that became famous for the image taken by the Hubble Space Telescope. Other striking objects include the Red Square Nebula, one of the few objects in astronomy to take on a square shape; and Westerhout 40, a massive nearby star-forming region consisting of a molecular cloud and an H II region.