sections 23-25 powerpoint
... gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, along with gas or dust, dominated by two (or more) spiral arms. Irregular galaxy (Ir). A galaxy containing m ...
... gas or dust. Spiral Galaxy (S). A galaxy with a spheroidal bulge of several million old low-mass stars and a flattened pancake-like disk of billions of old low-mass and young high-mass stars, along with gas or dust, dominated by two (or more) spiral arms. Irregular galaxy (Ir). A galaxy containing m ...
(Download from http://astronomy.nmsu.edu/astro/) c NMSU
... plot. For comparing the stock market you need to plot the value of the stocks versus the date. We call data of this type an “ordered pair”. Each data point requires a value for x (the date) and y (the value of the Dow Jones index). In the next table is the data for how the temperature changes with a ...
... plot. For comparing the stock market you need to plot the value of the stocks versus the date. We call data of this type an “ordered pair”. Each data point requires a value for x (the date) and y (the value of the Dow Jones index). In the next table is the data for how the temperature changes with a ...
PDF - NMSU Astronomy
... plot. For comparing the stock market you need to plot the value of the stocks versus the date. We call data of this type an “ordered pair”. Each data point requires a value for x (the date) and y (the value of the Dow Jones index). In the next table is the data for how the temperature changes with a ...
... plot. For comparing the stock market you need to plot the value of the stocks versus the date. We call data of this type an “ordered pair”. Each data point requires a value for x (the date) and y (the value of the Dow Jones index). In the next table is the data for how the temperature changes with a ...
2 Justification and benefits in joining TMT
... questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many decades to come; it can be a transformational experience for Chinese astronomy in terms of scienc ...
... questions with the next generation extremely large class telescopes such as the Thirty Meter Telescope (TMT). The Chinese participation in the TMT will place China in the forefront of astronomy for many decades to come; it can be a transformational experience for Chinese astronomy in terms of scienc ...
Astronomy WHS Sow
... System and large objects around other stars, disputes arose over what should constitute a planet. There was particular disagreement over whether an object should be considered a planet if it was part of a distinct population such as a belt, or if it was large enough to generate energy by the thermon ...
... System and large objects around other stars, disputes arose over what should constitute a planet. There was particular disagreement over whether an object should be considered a planet if it was part of a distinct population such as a belt, or if it was large enough to generate energy by the thermon ...
instructor notes: weeks 9/10
... “collisions” we are talking about events that take place over billions of years, not mere seconds or minutes. ...
... “collisions” we are talking about events that take place over billions of years, not mere seconds or minutes. ...
JENAM-2011 Book of abstracts
... The X-ray appearance of majority of normal galaxies is determined by radiation from accreting neutron stars and stellar mass black holes in X-ray binaries. Chandra and XMM-Newton observations revealed that their populations scale with the star-formation rate and stellar mass of the host galaxy. Thus ...
... The X-ray appearance of majority of normal galaxies is determined by radiation from accreting neutron stars and stellar mass black holes in X-ray binaries. Chandra and XMM-Newton observations revealed that their populations scale with the star-formation rate and stellar mass of the host galaxy. Thus ...
Distance to VY Canis Majoris with VERA
... feature at a LSR velocity of about 0.55 km s1 was analyzed to detect an annual parallax. This feature, the most blue-shifted discrete component, was stably detected at all epochs. It is the third-brightest maser component in the total-power spectrum, but in fact it is the second-brightest component ...
... feature at a LSR velocity of about 0.55 km s1 was analyzed to detect an annual parallax. This feature, the most blue-shifted discrete component, was stably detected at all epochs. It is the third-brightest maser component in the total-power spectrum, but in fact it is the second-brightest component ...
Giant molecular clouds in the Local Group galaxy M 33⋆⋆⋆
... at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this subsolar metallicity galaxy. The CPROPS (Cloud PROPertieS) algorithm was used to identify 337 GMCs in M 33, the largest sample ...
... at a distance of 840 kpc, is close enough for individual giant molecular clouds (GMCs) to be identified. The goal of this work is to study the properties of the GMCs in this subsolar metallicity galaxy. The CPROPS (Cloud PROPertieS) algorithm was used to identify 337 GMCs in M 33, the largest sample ...
Radio pulsars
... • The ratio of period P to slowdown rate P gives an estimate of the pulsar age - typically 106 years. • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
... • The ratio of period P to slowdown rate P gives an estimate of the pulsar age - typically 106 years. • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
– 1 – 1. Galaxy Observations 1.1.
... intermittant public releases of hundreds of thousands of spectra, and precision 5 color photometry, has been revolutionary. The SDSS magnitude limit means that galaxies with redshifts beyond z ∼ 0.3 are difficult to reach, but out to that distance, the SDSS changed the nature of the field. The major ...
... intermittant public releases of hundreds of thousands of spectra, and precision 5 color photometry, has been revolutionary. The SDSS magnitude limit means that galaxies with redshifts beyond z ∼ 0.3 are difficult to reach, but out to that distance, the SDSS changed the nature of the field. The major ...
An Atlas of Stellar Spectra
... of spectral classification is similar. The observer must use good judgment as to the definiteness with which the identification can be made from the features available; but good judgment is necessary in any case, whether the decision is made from the general appearance or from more objective measure ...
... of spectral classification is similar. The observer must use good judgment as to the definiteness with which the identification can be made from the features available; but good judgment is necessary in any case, whether the decision is made from the general appearance or from more objective measure ...
the fixed stars
... arbitrators, but exposes to cruel and severe trials. By the Kabalists this constellation is associated with the Hebrew letter Shin and the 22nd Tarot Trump, The Fool". (Robson). Rising: Cepheus will not engender dispositions inclined to sport. He fashions faces marked by a stern demeanour, and mould ...
... arbitrators, but exposes to cruel and severe trials. By the Kabalists this constellation is associated with the Hebrew letter Shin and the 22nd Tarot Trump, The Fool". (Robson). Rising: Cepheus will not engender dispositions inclined to sport. He fashions faces marked by a stern demeanour, and mould ...
Observations of Jets and Outflows from Young Stars
... of protostellar outflows, and the measurement of the emission and absorption spectra of some HH objects in the UV (Section 2). At visual and near-IR wavelengths, the formats of detectors has continued to increase with pixel counts doubling approximately every two years. This has led to the first com ...
... of protostellar outflows, and the measurement of the emission and absorption spectra of some HH objects in the UV (Section 2). At visual and near-IR wavelengths, the formats of detectors has continued to increase with pixel counts doubling approximately every two years. This has led to the first com ...
The physics and modes of star cluster formation: observations
... infrared wavelengths (e.g. Green & Lada 1996; White et al. 2007). Infrared spectroscopic surveys, especially those done with multi-object spectrographs, can be used to identify accreting objects in a cluster field. However, such observations can be time-consuming and even prohibitive for faint member ...
... infrared wavelengths (e.g. Green & Lada 1996; White et al. 2007). Infrared spectroscopic surveys, especially those done with multi-object spectrographs, can be used to identify accreting objects in a cluster field. However, such observations can be time-consuming and even prohibitive for faint member ...
A Zoo of Galaxies - Cambridge University Press
... In his 1927 defence of the classification scheme, Hubble claimed to have examined “upward of a thousand galaxies” in its construction. However for true physical understanding of a galaxy, more than just an image is required – we also need an estimate of its distance in order to reveal its size and ma ...
... In his 1927 defence of the classification scheme, Hubble claimed to have examined “upward of a thousand galaxies” in its construction. However for true physical understanding of a galaxy, more than just an image is required – we also need an estimate of its distance in order to reveal its size and ma ...
PhD thesis - Hamburger Sternwarte
... First, a transformation equation was derived for the HRT S-intex to be the Mount Wilson S-index so that it is possible to compare the activity levels of stars observed at different observatories. Thereafter, new photospheric flux corrections which depend on the colour index B − V for Ca H+K lines we ...
... First, a transformation equation was derived for the HRT S-intex to be the Mount Wilson S-index so that it is possible to compare the activity levels of stars observed at different observatories. Thereafter, new photospheric flux corrections which depend on the colour index B − V for Ca H+K lines we ...
Downloaded - Royal Society Open Science
... Decades of unsuccessful attempts to find planets around other Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around the millisecond pulsar PSR B1257+12 were the first confidently reported extrasolar planets to withstand enduring s ...
... Decades of unsuccessful attempts to find planets around other Sun-like stars preceded the unexpected 1992 discovery of planetary bodies orbiting a pulsar [1,2]. The three planets around the millisecond pulsar PSR B1257+12 were the first confidently reported extrasolar planets to withstand enduring s ...
Giant star seismology
... Asteroseismology – the study of global properties of stars and their internal structure through their global intrinsic oscillations – is already more than a century old. An early remarkable result was obtained for Cepheids revealing the period-luminosity relation (Leavitt and Pickering, 1912), which ...
... Asteroseismology – the study of global properties of stars and their internal structure through their global intrinsic oscillations – is already more than a century old. An early remarkable result was obtained for Cepheids revealing the period-luminosity relation (Leavitt and Pickering, 1912), which ...
Ursa Minor
Ursa Minor (Latin: ""Smaller She-Bear"", contrasting with Ursa Major), also known as the Little Bear, is a constellation in the northern sky. Like the Great Bear, the tail of the Little Bear may also be seen as the handle of a ladle, hence the name Little Dipper. It was one of the 48 constellations listed by the 2nd-century astronomer Ptolemy, and remains one of the 88 modern constellations. Ursa Minor has traditionally been important for navigation, particularly by mariners, due to Polaris being the North Star.Polaris, the brightest star in the constellation, is a yellow-white supergiant and the brightest Cepheid variable star in the night sky, ranging from apparent magnitude 1.97 to 2.00. Beta Ursae Minoris, also known as Kochab, is an aging star that has swollen and cooled to become an orange giant with an apparent magnitude of 2.08, only slightly fainter than Polaris. Kochab and magnitude 3 Gamma Ursae Minoris have been called the ""guardians of the pole star"". Planets have been detected orbiting four of the stars, including Kochab. The constellation also contains an isolated neutron star—Calvera—and H1504+65, the hottest white dwarf yet discovered with a surface temperature of 200,000 K.