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Annual report 2004 - Département d`Astrophysique, Géophysique et
... In the framework of a long-term spectroscopic and photometric monitoring of slowly pulsating B stars we studied thoroughly the northern target star HD 147394. We performed an end-to-end analysis, consisting of a frequency analysis, a mode identification from line-profile variations and a comparison ...
... In the framework of a long-term spectroscopic and photometric monitoring of slowly pulsating B stars we studied thoroughly the northern target star HD 147394. We performed an end-to-end analysis, consisting of a frequency analysis, a mode identification from line-profile variations and a comparison ...
ASTRONOMY 113 Laboratory Lab 5: Spectral Classification of the
... Some of the most beautiful objects in the sky are star clusters, groups of stars ranging in number from a few hundreds of stars ("open clusters") to a few million stars ("globular star clusters"). All of the stars in these clusters are bound to each other by gravity. Star clusters are also valuable ...
... Some of the most beautiful objects in the sky are star clusters, groups of stars ranging in number from a few hundreds of stars ("open clusters") to a few million stars ("globular star clusters"). All of the stars in these clusters are bound to each other by gravity. Star clusters are also valuable ...
Searching for the oldest, most metal-poor stars in the SkyMapper Survey
... is surveyed in the different filters, which only allows light with certain wavelengths to pass through. The calcium absorption line (Ca II K line) region around 3993 Å is observed with the narrow v filter. This way, metallicity information is gained by photometrically measuring the strength of the ...
... is surveyed in the different filters, which only allows light with certain wavelengths to pass through. The calcium absorption line (Ca II K line) region around 3993 Å is observed with the narrow v filter. This way, metallicity information is gained by photometrically measuring the strength of the ...
Main-Sequence Stars and the Sun
... relation to the surface temperature of the star is as follows. Hydrogen Balmer lines. Absorption lines caused by hydrogen atoms that are initially in the first excited state (see Chapter 1) are referred to as Balmer lines. At low surface temperatures, most of the hydrogen atoms are in the ground sta ...
... relation to the surface temperature of the star is as follows. Hydrogen Balmer lines. Absorption lines caused by hydrogen atoms that are initially in the first excited state (see Chapter 1) are referred to as Balmer lines. At low surface temperatures, most of the hydrogen atoms are in the ground sta ...
doc - Pocket Stars
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
... an improved fix from two or more LOPs. You can select from amongst the previously acquired observations by checking the associated checkbox. The results are shown in red text in the lower left corner. These include: ...
black hole
... The first white dwarf discovered was the faint companion to the well-known star Sirius. Sirius, the brightest star in the sky, is a visual binary star, the most luminous member of which is Sirius A. The white dwarf, Sirius B, is 10,000 times fainter than Sirius A. ...
... The first white dwarf discovered was the faint companion to the well-known star Sirius. Sirius, the brightest star in the sky, is a visual binary star, the most luminous member of which is Sirius A. The white dwarf, Sirius B, is 10,000 times fainter than Sirius A. ...
Journey through the cosmos
... When you look at the night sky, you can see only about three thousand stars of our own Galaxy with the naked eye. The darker the skies, the more stars you can see. Of course, there are billions more stars but they are so far away. You can see stars because they are luminous, which means that they gi ...
... When you look at the night sky, you can see only about three thousand stars of our own Galaxy with the naked eye. The darker the skies, the more stars you can see. Of course, there are billions more stars but they are so far away. You can see stars because they are luminous, which means that they gi ...
Nebula
... originates from a similarity in appearance to giant planets when viewed through a small optical telescope and is unrelated to planets of the solar system. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion ...
... originates from a similarity in appearance to giant planets when viewed through a small optical telescope and is unrelated to planets of the solar system. They are a relatively short-lived phenomenon, lasting a few tens of thousands of years, compared to a typical stellar lifetime of several billion ...
Astronomy Astrophysics NGC 7419 as a template for red supergiant clusters &
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
CW9_MOST_GSphot_RK_v1
... • exposure time is usually 1.5 sec (range from 0.3 to 1.5 applied) • no images are recovered, the image data is processed on board: a mean background value is removed and the signal is the sum of high signal pixels (exceeding the background and a 20 ADU threshold) • for the brightest guide stars noi ...
... • exposure time is usually 1.5 sec (range from 0.3 to 1.5 applied) • no images are recovered, the image data is processed on board: a mean background value is removed and the signal is the sum of high signal pixels (exceeding the background and a 20 ADU threshold) • for the brightest guide stars noi ...
Determination of kinetic energies of stars using Hipparcos data *
... constituent in proper motions has a peculiar or random nature. A drastic change in residual spatial velocity can be observed when crossing from the F to G spectrum. The modification of kinematic characteristics within this spectral range was observed long time ago by Parenago (Parenago P.P. 1954). ...
... constituent in proper motions has a peculiar or random nature. A drastic change in residual spatial velocity can be observed when crossing from the F to G spectrum. The modification of kinematic characteristics within this spectral range was observed long time ago by Parenago (Parenago P.P. 1954). ...
A historical perspective on the discovery of neutron stars
... Search for a neutron star in the Crab nebula The Crab nebula was observed during a lunar occultation on 7 July 1964. The size of the X-ray source was estimated as 1 light-year∼ 1013 km (size of the nebula 11 ly). This was much larger than the typical size of a neutron star (10-20 km). In 1965 Antho ...
... Search for a neutron star in the Crab nebula The Crab nebula was observed during a lunar occultation on 7 July 1964. The size of the X-ray source was estimated as 1 light-year∼ 1013 km (size of the nebula 11 ly). This was much larger than the typical size of a neutron star (10-20 km). In 1965 Antho ...
StellarManual
... implicit measure of intrinsic brightness and how much energy a star is releasing per second (luminosity). Thus: Avior (m = 1.9) and Alkaid (m = 1.9) appear to be the same brightness, but Avior (M = -4.8) emits more energy than Alkaid (M = -1.8). Barnard’s Star (m = 9.5) appears brighter than Wolf 35 ...
... implicit measure of intrinsic brightness and how much energy a star is releasing per second (luminosity). Thus: Avior (m = 1.9) and Alkaid (m = 1.9) appear to be the same brightness, but Avior (M = -4.8) emits more energy than Alkaid (M = -1.8). Barnard’s Star (m = 9.5) appears brighter than Wolf 35 ...
A-level Physics (Specification A) Teacher guide Teacher guide
... refraction eventually, in the eyepiece used to view the final image. The objective mirror is ‘exposed’, but the objective lens in a refractor is protected as it is inside a closed container. Overall however, it is clear that the reflector has the edge. One common misconception associated with the se ...
... refraction eventually, in the eyepiece used to view the final image. The objective mirror is ‘exposed’, but the objective lens in a refractor is protected as it is inside a closed container. Overall however, it is clear that the reflector has the edge. One common misconception associated with the se ...
Chapter 16--Properties of Stars
... century, humans classified stars primarily by their brightness and location in our sky. The names of the brightest stars within each constellation still bear Greek letters designating their order of brightness. For example, the brightest star in the constellation Centaurus is Alpha Centauri, the sec ...
... century, humans classified stars primarily by their brightness and location in our sky. The names of the brightest stars within each constellation still bear Greek letters designating their order of brightness. For example, the brightest star in the constellation Centaurus is Alpha Centauri, the sec ...
FREE Sample Here
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
... Answer: It means that when we look at a distant object, we see it as it was some time in the past, rather than as it is now. This is because the light we see has taken time to travel from the object to us. 3) Starting from the Big Bang, briefly explain how our solar system came to contain the chemic ...
The Halo of the Milky Way
... The spheroid population may be triaxial with a major axis oriented 65◦ from the line of sight from the Sun to the Galactic center. This is approximately perpendicular to the Galactic bar. This is surprising since one typically expects bars to have an angular pattern speed larger than could be sustai ...
... The spheroid population may be triaxial with a major axis oriented 65◦ from the line of sight from the Sun to the Galactic center. This is approximately perpendicular to the Galactic bar. This is surprising since one typically expects bars to have an angular pattern speed larger than could be sustai ...
Downloadable Full Text
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
... The UFD Reticulum II (Ret II) was recently discovered with Dark Energy Survey data12,13 and confirmed to be one of the most metal-poor galaxies known14. On 1-4 Oct 2015, we obtained high-resolution spectra of the nine brightest member stars in Ret II (see Table 1, Extended Data Figure 1). The abunda ...
Cassiopeia (constellation)
![](https://commons.wikimedia.org/wiki/Special:FilePath/ConstellationCassiopeia.jpg?width=300)
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.