:KDWLV/LJKW" (OHFWURPDJQHWLF:DYH7KHRU\
... Since silicon photodiodes are more sensitive to light at the red end of the spectrum than to light at the blue end, radiometric detectors filter the incoming light to even out the responsivity, producing a “flat response”. This is important for accurate radiometric measurements, because the spectru ...
... Since silicon photodiodes are more sensitive to light at the red end of the spectrum than to light at the blue end, radiometric detectors filter the incoming light to even out the responsivity, producing a “flat response”. This is important for accurate radiometric measurements, because the spectru ...
HI in Early-type Galaxies
... event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI is in an elongated structure parallel to the optical major axis. Most of this gas is rotating in a reas ...
... event. A good example of this is NGC 5266 (Figure 4; see Morganti et al. 1997a). This is a minor-axis dust-lane elliptical with a large amount of HI (∼1010 M¯ , MHI /LB ∼ 0 · 2). Almost all the HI is in an elongated structure parallel to the optical major axis. Most of this gas is rotating in a reas ...
the mass-loss return from evolved stars to the large
... et al. 2003). Further, the often unknown extent of extinction by intervening dust hampers precise distance determinations, which, in turn, affects determining AGB star luminosities. Blommaert et al. (2006) studied the mass loss of AGB stars in the Galactic Bulge; however, their surveys did not inclu ...
... et al. 2003). Further, the often unknown extent of extinction by intervening dust hampers precise distance determinations, which, in turn, affects determining AGB star luminosities. Blommaert et al. (2006) studied the mass loss of AGB stars in the Galactic Bulge; however, their surveys did not inclu ...
The far future of exoplanet direct characterization
... their transits in front of stars (Arnold, 2005); this kind of detection would be improved by resolving the stellar disc. 4. The Very Long-Term Perspective If around 2020–2030 we have found a promising biomarker candidate on a nearby planet [for instance, around Alpha Centauri (Guedes et al., 2008)], ...
... their transits in front of stars (Arnold, 2005); this kind of detection would be improved by resolving the stellar disc. 4. The Very Long-Term Perspective If around 2020–2030 we have found a promising biomarker candidate on a nearby planet [for instance, around Alpha Centauri (Guedes et al., 2008)], ...
age of the universe.
... a Doppler shift of the random motions of galaxies. an aging of light as the universe ages. space itself expanding with time, stretching light. the result of the Milky Way’s position at the center. being due to the temperature differences in the early and late universe. ...
... a Doppler shift of the random motions of galaxies. an aging of light as the universe ages. space itself expanding with time, stretching light. the result of the Milky Way’s position at the center. being due to the temperature differences in the early and late universe. ...
MS Word
... poll. Note the + label on the terminal. This connection terminal would be placed on to a positive (+) charged poll. A red marked connection terminal would be placed on to a negative (-) charged poll. Assembled Fan/ Motor Unit: The motor should always remain in the stand for safety purposes. ...
... poll. Note the + label on the terminal. This connection terminal would be placed on to a positive (+) charged poll. A red marked connection terminal would be placed on to a negative (-) charged poll. Assembled Fan/ Motor Unit: The motor should always remain in the stand for safety purposes. ...
Polarization Experiment
... The time for continuously using the sodium lamp tube should not exceed 4 hours. When the sodium lamp is being used for a long period of time, the electric fan must be used, or the sodium lamp should be turned off for 10-15 minutes so as to get it cooled before using it again. ...
... The time for continuously using the sodium lamp tube should not exceed 4 hours. When the sodium lamp is being used for a long period of time, the electric fan must be used, or the sodium lamp should be turned off for 10-15 minutes so as to get it cooled before using it again. ...
The University of Sydney Page
... Very low mass stars Very low mass stars (mass less than about 0.4 solar masses) are different in one important respect from heavier stars: their interiors are fully convective. The fused helium is stirred through the whole star, so it has the whole of its hydrogen mass to prolong its stay on the ma ...
... Very low mass stars Very low mass stars (mass less than about 0.4 solar masses) are different in one important respect from heavier stars: their interiors are fully convective. The fused helium is stirred through the whole star, so it has the whole of its hydrogen mass to prolong its stay on the ma ...
Astroparticle physics A.M. van den Berg () O. Scholten
... - Universe is hot, expanding plasma of radiation & relativistic particles - roughly equal # electrons, positrons, (anti)neutrinos, and photons - nucleons outnumbered by more than a billion to one ...
... - Universe is hot, expanding plasma of radiation & relativistic particles - roughly equal # electrons, positrons, (anti)neutrinos, and photons - nucleons outnumbered by more than a billion to one ...
SGHS Faulkes ASISTM Star Cluster Photometry
... This will give you a set of visible magnitudes V so you will then have a B and V value for each star. Note: It is very important that you match the B and V values for each star in each image. The B value you measured for star 1 must be recorded with the V value for that same star. The spreadsheet I ...
... This will give you a set of visible magnitudes V so you will then have a B and V value for each star. Note: It is very important that you match the B and V values for each star in each image. The B value you measured for star 1 must be recorded with the V value for that same star. The spreadsheet I ...
Lecture 1 - Simon P Driver
... • The GAMA9hr field is at RA=9h and Dec=0o, es1mate: – When would be the best date to observe this field? – If observed from the Anglo-‐Australian Telescope, how long would this object be at more ...
... • The GAMA9hr field is at RA=9h and Dec=0o, es1mate: – When would be the best date to observe this field? – If observed from the Anglo-‐Australian Telescope, how long would this object be at more ...
Sternentstehung - Star Formation
... - Deviate from spherical symmetry. Disks are known for low-mass star formation. High accretion rates necessary. - Coalescence of low- to intermediate-mass stars at the center of ...
... - Deviate from spherical symmetry. Disks are known for low-mass star formation. High accretion rates necessary. - Coalescence of low- to intermediate-mass stars at the center of ...
Paper II - van Werkhoven, Kenworthy and Mamajek (2014)
... where P0 is the nominal period and Ṗ the time-derivative of the period. This model is fitted to the data using the Nelder–Mead fitting algorithm (Nelder & Mead 1965). Our analysis shows that the bestfitting periods and their amplitudes differ significantly from year to year (see Table 1). Furthermo ...
... where P0 is the nominal period and Ṗ the time-derivative of the period. This model is fitted to the data using the Nelder–Mead fitting algorithm (Nelder & Mead 1965). Our analysis shows that the bestfitting periods and their amplitudes differ significantly from year to year (see Table 1). Furthermo ...
PDF only - at www.arxiv.org.
... the main disk plane (Fig.1B) and is more closely aligned with the inner planet b Pic b and a secondary disk seen in scattered light (5,9). The CO J=3-‐2 emission totals 7.6±0.8x10-‐20 W/ ...
... the main disk plane (Fig.1B) and is more closely aligned with the inner planet b Pic b and a secondary disk seen in scattered light (5,9). The CO J=3-‐2 emission totals 7.6±0.8x10-‐20 W/ ...
X-ray effects on protoplanetary disks
... X-rays are the principal source of disk ionization YSO X-ray ionization rate dominates CRs in the disk by 108 for 1Mo PMS star at 1 AU: z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-20 keV) X-rays ...
... X-rays are the principal source of disk ionization YSO X-ray ionization rate dominates CRs in the disk by 108 for 1Mo PMS star at 1 AU: z = 6x10-9 (Lx/2x1030 erg s-1) (r/1 AU)-2 s-1 The ionization fraction is uncertain due to recombination processes. Hard (5-20 keV) X-rays ...
White Dwarf Stars - Stellar Physics Department
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
... H for magnetic white dwarfs that do show any detectable polarization. P for polarized magnetic white dwarfs. V for variable white dwarfs. And finally to complete the classification, a temperature index can follow their spectral classification. This index is defined as θ = 50400/Teff . Therefore, a w ...
Ray Diagrams
... Imaginary light rays extended behind mirrors are called sight lines. The image is virtual since it is formed by imaginary sight lines, not real light rays. J.M. Gabrielse ...
... Imaginary light rays extended behind mirrors are called sight lines. The image is virtual since it is formed by imaginary sight lines, not real light rays. J.M. Gabrielse ...
ASTR1102-002 Potentially useful facts and mathematical relations
... parallax of 0.15 arcsec/yr. Which star is moving through space with the faster speed? a. Star “A” is moving faster than star “B”. b. Star “B” is moving faster than star “A”. c. The stars are moving through space at the same speed. d. None of the above. (Briefly explain.) ANS: ...
... parallax of 0.15 arcsec/yr. Which star is moving through space with the faster speed? a. Star “A” is moving faster than star “B”. b. Star “B” is moving faster than star “A”. c. The stars are moving through space at the same speed. d. None of the above. (Briefly explain.) ANS: ...
Three models of light
... the image is called real. • If a screen is put at the real image, the rays will scatter in all directions and an image can be seen on the screen, just as if it were a ...
... the image is called real. • If a screen is put at the real image, the rays will scatter in all directions and an image can be seen on the screen, just as if it were a ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.