- ANU Repository
... and is essentially zero at 4 R⊕ , although we identify three giant planet candidates other than the previously confirmed Kepler-45b. There is suggestive but not significant evidence that the radius distribution varies with orbital period. The distribution with logarithmic orbital period is flat except ...
... and is essentially zero at 4 R⊕ , although we identify three giant planet candidates other than the previously confirmed Kepler-45b. There is suggestive but not significant evidence that the radius distribution varies with orbital period. The distribution with logarithmic orbital period is flat except ...
Stellar evolution - Statistical Physics Group
... used system involves three bands in the ultra-violet, blue and yellow regions of the spectrum and the magnitudes? corresponding to these measurements are denoted by U , B and V . T h e difference between any two magnitudes is called a colour index; if stars radiated like black bodies, colour index w ...
... used system involves three bands in the ultra-violet, blue and yellow regions of the spectrum and the magnitudes? corresponding to these measurements are denoted by U , B and V . T h e difference between any two magnitudes is called a colour index; if stars radiated like black bodies, colour index w ...
Classification of Variable Stars
... Luminous Blue Variables (LBVs)/ S Dor Stars .............................................................................. 21 ...
... Luminous Blue Variables (LBVs)/ S Dor Stars .............................................................................. 21 ...
The Norma cluster (ACO3627) – II. The near-infrared Ks
... seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded to obtain a better fit, particularly in cD clusters. The Schechter parameters have also been found to vary depending on the region sampled within the cluster, the size of the area and the limitin ...
... seem to have a steeper bright end than those without cD galaxies. Often the brightest galaxy is excluded to obtain a better fit, particularly in cD clusters. The Schechter parameters have also been found to vary depending on the region sampled within the cluster, the size of the area and the limitin ...
Astronomy 250 - University of Victoria
... and find the average brightness from those 10 observations. However, you notice that the brightness changes slightly in each image, which means that your average is not infinitely precise. Thus, you must also quantify the spread around this average in order to understand how well the average is know ...
... and find the average brightness from those 10 observations. However, you notice that the brightness changes slightly in each image, which means that your average is not infinitely precise. Thus, you must also quantify the spread around this average in order to understand how well the average is know ...
Astronomy Chapter 17 – Galaxies A. Main Ideas 1. Discovering
... use the method of standard candles to measure the distance to distant galaxies. Using the inverse-square law and the known luminosity of Cepheid variables scientists are able to reasonable measurements of the distances involved. • Redshift and the Hubble Law ⇒ In the 1920s, astronomers discovered th ...
... use the method of standard candles to measure the distance to distant galaxies. Using the inverse-square law and the known luminosity of Cepheid variables scientists are able to reasonable measurements of the distances involved. • Redshift and the Hubble Law ⇒ In the 1920s, astronomers discovered th ...
binary stars instructor notes
... The equation: M = E – e sin E is called Kepler’s Equation, which relates the eccentric anomaly E to the mean anomaly M. M is simple to calculate since it represents the amount of orbit swept out over a time interval t relative to the orbital period P, i.e. M = 2πt/P, where M is in radians. M is the ...
... The equation: M = E – e sin E is called Kepler’s Equation, which relates the eccentric anomaly E to the mean anomaly M. M is simple to calculate since it represents the amount of orbit swept out over a time interval t relative to the orbital period P, i.e. M = 2πt/P, where M is in radians. M is the ...
Red supergiants around the obscured open cluster Stephenson 2
... 3. We selected stars with infrared reddening-free parameter, QIR = (J − H) − 1.8 × (H − KS ), typical of RSGs: 0.1 ≤ QIR ≤ 0.4. Though some RSGs have QIR outside this range (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our ta ...
... 3. We selected stars with infrared reddening-free parameter, QIR = (J − H) − 1.8 × (H − KS ), typical of RSGs: 0.1 ≤ QIR ≤ 0.4. Though some RSGs have QIR outside this range (cf. Messineo et al. 2012), this cut selects most RSGs, while leaving out low-luminosity red stars. The vast majority of our ta ...
3D Tour of the Universe Template
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
... regions, resulting in the formation of new young stars. As is common in these kinds of encounters, spiral structure was induced in the more massive galaxy. M51 is an easily found astronomical showpiece if the sky is dark, where suggestions of its spiral arms may be visible. As is also common with th ...
Star Formation in the Rosette Complex
... α = 0.4 model for the temperature gradient in the nebula cavity which, interestingly, could not be adjusted to the observed IRAS emission. Instead, they found that this temperature gradient was better adjusted to α = 0.05 for r < 47′ and α = 0.2 for 47′ < r < 65′ (see also Section 3.2). The pioneeri ...
... α = 0.4 model for the temperature gradient in the nebula cavity which, interestingly, could not be adjusted to the observed IRAS emission. Instead, they found that this temperature gradient was better adjusted to α = 0.05 for r < 47′ and α = 0.2 for 47′ < r < 65′ (see also Section 3.2). The pioneeri ...
ancient cultures 114 - Stellenbosch University
... The earliest texts indicating Babylonian interest in celestial bodies dates to approximately 1700 BCE (Bienkowski & Millard 2000: 40). The interest during this time, however, seems to be purely astrological; the texts all being what are known as “omen” texts. A standard series of these omen texts wa ...
... The earliest texts indicating Babylonian interest in celestial bodies dates to approximately 1700 BCE (Bienkowski & Millard 2000: 40). The interest during this time, however, seems to be purely astrological; the texts all being what are known as “omen” texts. A standard series of these omen texts wa ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... [Fe/H]≤ −3 have been observed, and 10 of them are found to be CEMP-no stars. This gives FCEMP (< −3) ≈ 42%. However, when we consider individual dwarf galaxies, the fractions are highly variable. The carbon measurements in the least luminous ultra-faint dwarf galaxies, log(L/L# ) < 4.0 (shown in Fig ...
... [Fe/H]≤ −3 have been observed, and 10 of them are found to be CEMP-no stars. This gives FCEMP (< −3) ≈ 42%. However, when we consider individual dwarf galaxies, the fractions are highly variable. The carbon measurements in the least luminous ultra-faint dwarf galaxies, log(L/L# ) < 4.0 (shown in Fig ...
Abd al-Rahman al-Sufi and his book of the fixed stars: a journey of
... Beirut. Finally I would like to thank all people and especially my family for their help, support and patience during the time I spent working on this project. ...
... Beirut. Finally I would like to thank all people and especially my family for their help, support and patience during the time I spent working on this project. ...
Ptolemy: on trial for fraud
... /6°) would receive rounded up or down measurements from one category each (from 5, 25, 35 and 55 min), increasing their membership by half. Hence, if the instrument(s) gave readings only in sixths and quarters of a degree, we could expect peaks in the distribution of the reported measurements at 0 a ...
... /6°) would receive rounded up or down measurements from one category each (from 5, 25, 35 and 55 min), increasing their membership by half. Hence, if the instrument(s) gave readings only in sixths and quarters of a degree, we could expect peaks in the distribution of the reported measurements at 0 a ...
Cassiopeia (constellation)
Cassiopeia is a constellation in the northern sky, named after the vain queen Cassiopeia in Greek mythology, who boasted about her unrivalled beauty. Cassiopeia was one of the 48 constellations listed by the 2nd-century Greek astronomer Ptolemy, and it remains one of the 88 modern constellations today. It is easily recognizable due to its distinctive 'M' shape when in upper culmination but in higher northern locations when near lower culminations in spring and summer it has a 'W' shape, formed by five bright stars. It is bordered by Andromeda to the south, Perseus to the southeast, and Cepheus to the north. It is opposite the Big Dipper.In northern locations above 34ºN latitude it is visible year-round and in the (sub)tropics it can be seen at its clearest from September to early November in its characteristic 'M' shape. Even in low southern latitudes below 25ºS is can be seen low in the North.