Stellarium User Guide
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
... scipting facility is Stellarium’s version of a “Presentation”, a feature that may be used to run an astronomical or other presentation for instruction or entertainment from within the Stellarium program. The original Stratoscript was quite limited in what it could do so a new Stellarium Scripting Sy ...
The Evolution of Isotope Ratios in the Milky Way Galaxy
... medium (ISM), which contains elements with the abundance pattern of the Galaxy at the time when the stars formed. The He core mass is set as Mremnant = 0.459 and 0.473M⊙ for 0.7 and 0.9M⊙ , respectively. Asymptotic Giant Branch (AGB) stars — Stars with initial masses between about 0.8 − 8M⊙ (dependi ...
... medium (ISM), which contains elements with the abundance pattern of the Galaxy at the time when the stars formed. The He core mass is set as Mremnant = 0.459 and 0.473M⊙ for 0.7 and 0.9M⊙ , respectively. Asymptotic Giant Branch (AGB) stars — Stars with initial masses between about 0.8 − 8M⊙ (dependi ...
Pulsed Accretion in the Young Binary &
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
... these have been identified as possible sites for the study of early stellar evolution and planetary formation. Stellar formation starts when a gravitational collapse is triggered in dense regions of slowly rotating gaseous clouds. As the gravitational force depends on the inverse-square of the dista ...
solon irving bailey - National Academy of Sciences
... elevated station might be maintained. Thus the problem was solved by the construction of a mule-path to the summit. A vivid description of this project is given in Harvard Annals 39, the first volume of the Peruvian Meteorology. After Professor Bailey and his party had passed eight consecutive days ...
... elevated station might be maintained. Thus the problem was solved by the construction of a mule-path to the summit. A vivid description of this project is given in Harvard Annals 39, the first volume of the Peruvian Meteorology. After Professor Bailey and his party had passed eight consecutive days ...
Galaxy Sorting
... disks. Irregular galaxies appear chaotic, and often have many bright, young stars, the result of recent bursts of intense star formation. For many years, astronomers thought the dissimilarities between galaxy types reflected different conditions present in each when they originally formed. Put an ...
... disks. Irregular galaxies appear chaotic, and often have many bright, young stars, the result of recent bursts of intense star formation. For many years, astronomers thought the dissimilarities between galaxy types reflected different conditions present in each when they originally formed. Put an ...
The Ages of Stars
... Yet age lies at the heart of stellar evolution, for how can there be evolution About Stellar Ages? without the passage of time? Sometimes our desire to know ages is satisfied if we (see p. 46) can place events in the correct sequence and understand the relative duration of phases. But often we need ...
... Yet age lies at the heart of stellar evolution, for how can there be evolution About Stellar Ages? without the passage of time? Sometimes our desire to know ages is satisfied if we (see p. 46) can place events in the correct sequence and understand the relative duration of phases. But often we need ...
Reassessing the formation of the inner Oort cloud
... We re-examine the formation of the inner Oort comet cloud while the Sun was in its birth cluster with the aid of numerical simulations. This work is a continuation of an earlier study (Brasser et al., 2006) with several substantial modifications. First, the system consisting of stars, planets and co ...
... We re-examine the formation of the inner Oort comet cloud while the Sun was in its birth cluster with the aid of numerical simulations. This work is a continuation of an earlier study (Brasser et al., 2006) with several substantial modifications. First, the system consisting of stars, planets and co ...
- National Optical Astronomy Observatory
... magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movement is not the flow of iron directed by the magnetic fields. The nickel displays greater va ...
... magnetic field lines unless there was an indirect mechanism for their flow, namely, other materials that are directed by the magnetic field. The data seems to indicate that the mechanism for the nickel’s movement is not the flow of iron directed by the magnetic fields. The nickel displays greater va ...
structure and evolution of white dwarfs and their
... resolved by A.G. Clark in 1862 and the orbital period revealed to be 50 years. Later, the first spectroscopic study of the system by W.S. Adams revealed a great enigma. While the temperature of Sirius B was found to be higher than Sirius A, it was apparently 1000 times less luminous. This result cou ...
... resolved by A.G. Clark in 1862 and the orbital period revealed to be 50 years. Later, the first spectroscopic study of the system by W.S. Adams revealed a great enigma. While the temperature of Sirius B was found to be higher than Sirius A, it was apparently 1000 times less luminous. This result cou ...
Chemical analysis of 24 dusty (pre-) main
... Herbig Ae/Be (HAEBE) stars are generally thought to be the somewhat more massive analogues of the T Tauri stars, which are low-mass pre-main-sequence stars. They were first defined as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display ...
... Herbig Ae/Be (HAEBE) stars are generally thought to be the somewhat more massive analogues of the T Tauri stars, which are low-mass pre-main-sequence stars. They were first defined as a class in 1960 by Herbig, based on three observational criteria: the stars have spectral type A or earlier, display ...
Mathematica - Press Center
... All rights reserved. No part of this document may be reproduced, stored in a retrieval system, or transmitted in any form or by any means, electronic, mechani cal, photocopying, recording or otherwise, without the prior written permission of the author Terry Robb and Wolfram Research, Inc. Stellar S ...
... All rights reserved. No part of this document may be reproduced, stored in a retrieval system, or transmitted in any form or by any means, electronic, mechani cal, photocopying, recording or otherwise, without the prior written permission of the author Terry Robb and Wolfram Research, Inc. Stellar S ...
Galaxies
... arms are wound, with “a” being most tightly wound. The Andromeda Galaxy is an Sb. • Elliptical galaxies are denoted by “E”, with a number from 0-7 indicating how circular it appears. An example of this would be M87, which is an E0 galaxy. • Irregulars, such as the Small Magellanic Cloud, are denoted ...
... arms are wound, with “a” being most tightly wound. The Andromeda Galaxy is an Sb. • Elliptical galaxies are denoted by “E”, with a number from 0-7 indicating how circular it appears. An example of this would be M87, which is an E0 galaxy. • Irregulars, such as the Small Magellanic Cloud, are denoted ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... 5.3 O-rich and O-poor ω Cen stars and their CH(4300) and S(3839) spectral indices. . . . . . . . . . . . . 5.4 The difference in photometry of the ω Cen stars between van Leeuwen et al. (2000) and Bellini et al. (2009a). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...
... 5.3 O-rich and O-poor ω Cen stars and their CH(4300) and S(3839) spectral indices. . . . . . . . . . . . . 5.4 The difference in photometry of the ω Cen stars between van Leeuwen et al. (2000) and Bellini et al. (2009a). . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . ...
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.