Star Formation in the Local Milky Way
... 1978, Kroupa 2002, Chabrier 2003). In addition, infrared studies of local, very young star clusters provided independent determinations of the IMF over an even larger dynamic range in mass, from the deuterium burning limit to OB stars (e.g., Muench et al. 2002). These studies have found that the sha ...
... 1978, Kroupa 2002, Chabrier 2003). In addition, infrared studies of local, very young star clusters provided independent determinations of the IMF over an even larger dynamic range in mass, from the deuterium burning limit to OB stars (e.g., Muench et al. 2002). These studies have found that the sha ...
Chapter 6: Stellar Evolution (part 2)
... First observed visually on Feb. 24, 1987 in the LMC. Kind of unique light-curve and intrinsically dimmer, compared with the “normal” Type II SNe. Progenitor: B3 I blue supergiant (16-20 M ). The key evidence for the core collapse and the formation of a neutron star is the detection of the neutrinos ...
... First observed visually on Feb. 24, 1987 in the LMC. Kind of unique light-curve and intrinsically dimmer, compared with the “normal” Type II SNe. Progenitor: B3 I blue supergiant (16-20 M ). The key evidence for the core collapse and the formation of a neutron star is the detection of the neutrinos ...
How many stars are in the Milky Way Galaxy?
... 1: Draw and label diagrams of the Milky Way from top and side views, showing the major components. Indicate the approximate dimensions of the components and note the location of the Sun in each diagram. 2: Describe the galactic distribution of general interstellar material, nebulae, and open and glo ...
... 1: Draw and label diagrams of the Milky Way from top and side views, showing the major components. Indicate the approximate dimensions of the components and note the location of the Sun in each diagram. 2: Describe the galactic distribution of general interstellar material, nebulae, and open and glo ...
m/s
... the radial velocity variations are all accompained by changes in the shape of the spectral lines. Planets on the other hand cause an overall Doppler shift of the line without an accompanying change in the lines. Spectral line bisectors are a common way to measure line shapes ...
... the radial velocity variations are all accompained by changes in the shape of the spectral lines. Planets on the other hand cause an overall Doppler shift of the line without an accompanying change in the lines. Spectral line bisectors are a common way to measure line shapes ...
Celestial Sphere
... Declination (like latitude) is measured in degrees north or south of the Celestial equator. Right ascension (like longitude) is measured in units of hours, minutes, and seconds eastward from the position of the vernal equinox on the Celestial equator. The Vernal Equinox is the position of the Sun on ...
... Declination (like latitude) is measured in degrees north or south of the Celestial equator. Right ascension (like longitude) is measured in units of hours, minutes, and seconds eastward from the position of the vernal equinox on the Celestial equator. The Vernal Equinox is the position of the Sun on ...
Life Stages of High
... • Late life stages of high-mass stars are similar to those of low-mass stars: —Hydrogen core fusion (main sequence) ...
... • Late life stages of high-mass stars are similar to those of low-mass stars: —Hydrogen core fusion (main sequence) ...
Chapter 17 Star Stuff
... • He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium ...
... • He fuses into carbon in a shell around the carbon core, and H fuses to He in a shell around the helium ...
Measuring Starlight Deflection during the 2017 Eclipse: Repeating
... after totality begins. Then, 30 seconds later, the telescope will be repointed to the central eclipse field. Exposures here will be bracketed from 0.2 second to 1 second. After 60 seconds imaging the central eclipse field, the telescope will be repointed to the second reference field for the last 30 ...
... after totality begins. Then, 30 seconds later, the telescope will be repointed to the central eclipse field. Exposures here will be bracketed from 0.2 second to 1 second. After 60 seconds imaging the central eclipse field, the telescope will be repointed to the second reference field for the last 30 ...
preliminary version - University of Exeter
... IC 348 we took data on 15 consecutive nights, and repeated the observations many times within a single night. By contrast, the survey of Cohen et al. 2004[2] has much lower temporal density, and many nights can elapse between observations. Because CTTs are erratically variable with time-scales of or ...
... IC 348 we took data on 15 consecutive nights, and repeated the observations many times within a single night. By contrast, the survey of Cohen et al. 2004[2] has much lower temporal density, and many nights can elapse between observations. Because CTTs are erratically variable with time-scales of or ...
Slide 1
... •Endpoint of evolution for most stars •Homogeneous –Narrow mass distribution –Chemically pure layers ...
... •Endpoint of evolution for most stars •Homogeneous –Narrow mass distribution –Chemically pure layers ...
SciPoster_Jan2009
... 8’ long, is V1331 (Quanz et al. 2007). LDN 981 has a distance of 700 pc (Lee and Myers 1999). V1331 Cyg, which seems to be associated with LDN 981, has distances reported from 694 pc (Chavarria 1981) to 550 pc (Shevchenko et al. 1991). With V1331 Cyg having two rings of dust, it is suggested to be a ...
... 8’ long, is V1331 (Quanz et al. 2007). LDN 981 has a distance of 700 pc (Lee and Myers 1999). V1331 Cyg, which seems to be associated with LDN 981, has distances reported from 694 pc (Chavarria 1981) to 550 pc (Shevchenko et al. 1991). With V1331 Cyg having two rings of dust, it is suggested to be a ...
Pp 263-266 - Gravity From The Ground Up
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
... to somewhere between two and possibly three solar masses. Its actual value is not known: uncertainties in nuclear physics prevent reliable calculations. We have learned that neutron stars can only exist in a rather restricted range of masses, between perhaps 0.1 and two solar masses. In fact, their ...
two dozen compact sources and a massive disk
... theoretical papers in 1970s: – First appearance in a paper abstract: M. Disney (1975), “Boundary and Initial Conditions in Protostar Calculations” – First appearance in a paper title: Ferraioli & Virgopia (1979), “On the Mass Distribution Law of Systems of Protocluster Fragments” • Observational pap ...
... theoretical papers in 1970s: – First appearance in a paper abstract: M. Disney (1975), “Boundary and Initial Conditions in Protostar Calculations” – First appearance in a paper title: Ferraioli & Virgopia (1979), “On the Mass Distribution Law of Systems of Protocluster Fragments” • Observational pap ...
Next Generation Sunshine State Standards Chapter 24
... sizes, temperatures, and distances, so their apparent brightnesses vary widely. Apparent Magnitude Stars have been classified according to their apparent brightness since at least the second century BC, when Hipparchus placed about 850 of them into six categories based on his ability to see differen ...
... sizes, temperatures, and distances, so their apparent brightnesses vary widely. Apparent Magnitude Stars have been classified according to their apparent brightness since at least the second century BC, when Hipparchus placed about 850 of them into six categories based on his ability to see differen ...
Chapter 15 Surveying the Stars
... What are giants, supergiants, and white dwarfs? Off the Main Sequence • Stellar properties depend on both mass and age: Those that have finished fusing H to He in their cores are no longer on the main sequence. • All stars become larger and redder after exhausting their core hydrogen: giants and ...
... What are giants, supergiants, and white dwarfs? Off the Main Sequence • Stellar properties depend on both mass and age: Those that have finished fusing H to He in their cores are no longer on the main sequence. • All stars become larger and redder after exhausting their core hydrogen: giants and ...
The Bigger Picture - Astronomy and Astrophysics
... Hydrogen lines in the visible part of the spectrum (known as the Balmer Series) are created when a photon is absorbed by bouncing an electron from the 1st excited level to a higher excited level. • Photons with just the right energy to move an electron from the 1st excited state to the 2nd excited s ...
... Hydrogen lines in the visible part of the spectrum (known as the Balmer Series) are created when a photon is absorbed by bouncing an electron from the 1st excited level to a higher excited level. • Photons with just the right energy to move an electron from the 1st excited state to the 2nd excited s ...
Astronomical Motions I: The Night Sky
... divided the stars into six categories of brightness with the brightest stars called first magnitude, the next brightest second magnitude, and so on down to the faintest stars visible to the naked eye, sixth magnitude. The Greeks, as well as other peoples, arranged the stars into groupings which we c ...
... divided the stars into six categories of brightness with the brightest stars called first magnitude, the next brightest second magnitude, and so on down to the faintest stars visible to the naked eye, sixth magnitude. The Greeks, as well as other peoples, arranged the stars into groupings which we c ...
Cygnus (constellation)
Cygnus /ˈsɪɡnəs/ is a northern constellation lying on the plane of the Milky Way, deriving its name from the Latinized Greek word for swan. The swan is one of the most recognizable constellations of the northern summer and autumn, it features a prominent asterism known as the Northern Cross (in contrast to the Southern Cross). Cygnus was among the 48 constellations listed by the 2nd century astronomer Ptolemy, and it remains one of the 88 modern constellations.Cygnus contains Deneb, one of the brightest stars in the night sky and one corner of the Summer Triangle, as well as some notable X-ray sources and the giant stellar association of Cygnus OB2. One of the stars of this association, NML Cygni, is one of the largest stars currently known. The constellation is also home to Cygnus X-1, a distant X-ray binary containing a supergiant and unseen massive companion that was the first object widely held to be a black hole. Many star systems in Cygnus have known planets as a result of the Kepler Mission observing one patch of the sky, the patch is the area around Cygnus. In addition, most of the eastern part of Cygnus is dominated by the Hercules–Corona Borealis Great Wall, a giant galaxy filament that is the largest known structure in the observable universe; covering most of the northern sky.