Camelopardalis-Better-Know-A-Constellation
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
... • Although Camelopardalis is the 18th largest constellation, (757 sq. deg. ) it is not a particularly bright constellation, as the brightest stars are only of fourth magnitude. • β Camelopardalis is the brightest star, at apparent magnitude 4.03. This star is a double star, with components of magnit ...
A terrestrial planet candidate in a temperate orbit around Proxima
... days,3 and its quiescent activity levels and X-ray luminosity4 are comparable to the Sun’s. New observations reveal the presence of a small planet orbiting Proxima with a minimum mass of 1.3 Earth masses and an orbital period of ∼11.2 days. Its orbital semi-major axis is ∼ 0.05 AU, with an equilibri ...
... days,3 and its quiescent activity levels and X-ray luminosity4 are comparable to the Sun’s. New observations reveal the presence of a small planet orbiting Proxima with a minimum mass of 1.3 Earth masses and an orbital period of ∼11.2 days. Its orbital semi-major axis is ∼ 0.05 AU, with an equilibri ...
On the interpretation of stellar disc observations in terms of diameters
... tries to interpret lunar-occultation or interferometric data naively in terms of, e.g., a uniform disc would see the star first shrink A1 ! A2 from its real diameter 2R to a much smaller value and then expand again A2 ! A3 towards 2R when observed features approach full saturation. If the observ ...
... tries to interpret lunar-occultation or interferometric data naively in terms of, e.g., a uniform disc would see the star first shrink A1 ! A2 from its real diameter 2R to a much smaller value and then expand again A2 ! A3 towards 2R when observed features approach full saturation. If the observ ...
SXDS Highlights : Subaru / FOCAS Spectroscopy
... Results of “cloning” simulations show if there are large number of elliptical or bulge-dominated galaxies at z~3, they should be detected, and should be fitted well with large n-index. ...
... Results of “cloning” simulations show if there are large number of elliptical or bulge-dominated galaxies at z~3, they should be detected, and should be fitted well with large n-index. ...
StellarManual
... It is recommended that the think-pair-share method be employed for these questions. Teaching suggestions, and possibly hints, are provided for every question. A degree of difficulty (1 – 5; 1 being easy and 5 being difficult) is also provided for every question. ...
... It is recommended that the think-pair-share method be employed for these questions. Teaching suggestions, and possibly hints, are provided for every question. A degree of difficulty (1 – 5; 1 being easy and 5 being difficult) is also provided for every question. ...
Chapter 1
... specific features and goals, pushing the boundaries of infrared astronomy in either spatial resolution, sensitivity, and/or sky coverage. The contents of this thesis largely revolve around observations taken with most of the aforementioned infrared observational facilities. Here, we particularly men ...
... specific features and goals, pushing the boundaries of infrared astronomy in either spatial resolution, sensitivity, and/or sky coverage. The contents of this thesis largely revolve around observations taken with most of the aforementioned infrared observational facilities. Here, we particularly men ...
binary stars instructor notes
... stars in a system. If a binary is resolved and close enough for astrometry to detect the motion of the system barycentre, the individual masses for the stars can also be established. Luminosities can be derived for systems of established distance. Spectroscopic binaries place constraints on the mass ...
... stars in a system. If a binary is resolved and close enough for astrometry to detect the motion of the system barycentre, the individual masses for the stars can also be established. Luminosities can be derived for systems of established distance. Spectroscopic binaries place constraints on the mass ...
Carbon-enhanced metal-poor stars in dwarf galaxies
... log(L/L# ) < 4.0 (shown in Fig. 1 with red circles), are from high-resolution spectroscopic studies (see caption for references). Although less than 20 stars have been observed in these 4 systems, the overall frequency of CEMP-no stars is very high, and at [Fe/H]≤ −3, 5 out of 6 stars are CEMP-no st ...
... log(L/L# ) < 4.0 (shown in Fig. 1 with red circles), are from high-resolution spectroscopic studies (see caption for references). Although less than 20 stars have been observed in these 4 systems, the overall frequency of CEMP-no stars is very high, and at [Fe/H]≤ −3, 5 out of 6 stars are CEMP-no st ...
The Milky Way thin disk structure as revealed by stars and young
... when seen face-off, possess dusty and gaseous disks where stars are barely visible. On the other hand, when seen face-on, they exhibit quite spectacular structures in the form of gaseous and stellar spiral arms, bridges, inter-arm structures, knots, bifurcations, and so forth. These detailed shapes a ...
... when seen face-off, possess dusty and gaseous disks where stars are barely visible. On the other hand, when seen face-on, they exhibit quite spectacular structures in the form of gaseous and stellar spiral arms, bridges, inter-arm structures, knots, bifurcations, and so forth. These detailed shapes a ...
Stellar evolution – Part III of III - Inside Mines
... • The source of the star’s energy (He burning) is eventually exhausted inside the core, which is now composed of carbon and oxygen • The core begins to contract without outward thermal pressure of fusion process. The contraction leads to further heating of the core. • Similarly to the “hydrogen shel ...
... • The source of the star’s energy (He burning) is eventually exhausted inside the core, which is now composed of carbon and oxygen • The core begins to contract without outward thermal pressure of fusion process. The contraction leads to further heating of the core. • Similarly to the “hydrogen shel ...
The Age Distribution of Potential Intelligent Life in the Milky Way
... the Galaxy’s history we created a galactic chemical evolution model (GCEM) using the computer programming language MATLAB (MathWorks, 2015) to determine which areas of the Galaxy’s disk may have been the most hospitable to life and when. This GCEM incorporated interstellar gas, star formation, super ...
... the Galaxy’s history we created a galactic chemical evolution model (GCEM) using the computer programming language MATLAB (MathWorks, 2015) to determine which areas of the Galaxy’s disk may have been the most hospitable to life and when. This GCEM incorporated interstellar gas, star formation, super ...
Resume
... measurements and wavefront modelling to improve and troubleshoot the star profile structure. This was crucial to obtain the atmospheric seeing limited profile which improved the faint source detection sensitivity of the instrument. Accurate field of view distortions were also measured and constraine ...
... measurements and wavefront modelling to improve and troubleshoot the star profile structure. This was crucial to obtain the atmospheric seeing limited profile which improved the faint source detection sensitivity of the instrument. Accurate field of view distortions were also measured and constraine ...
Tip-tilt mirror and sensor configuration
... – Laser Tomography AO: Multiple laser guide stars, 1 DM, corrects cone effect. Narrow field. – Multi-conjugate AO: Multiple DMs, each optically conjugate to a different layer in atmosphere. Wider field of view. – Multi-object AO: Correct many individual objects, each over a small field. Each has ver ...
... – Laser Tomography AO: Multiple laser guide stars, 1 DM, corrects cone effect. Narrow field. – Multi-conjugate AO: Multiple DMs, each optically conjugate to a different layer in atmosphere. Wider field of view. – Multi-object AO: Correct many individual objects, each over a small field. Each has ver ...
The Clouds
... OB stars, producing very strong infrared emission in the fine-structure lines of oxygen and carbon. Although the massive stars are prominent and appear to re-structure the complex, giving it the V-shape, lower mass stars are present in great numbers throughout the clouds. Just behind the Orion Nebul ...
... OB stars, producing very strong infrared emission in the fine-structure lines of oxygen and carbon. Although the massive stars are prominent and appear to re-structure the complex, giving it the V-shape, lower mass stars are present in great numbers throughout the clouds. Just behind the Orion Nebul ...
The High Resolution Camera CXC Newsletter
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
... or outbursting (with subclasses short vs. long outbursts and activity periods). 129 sources could be classified as X-ray binaries due to their position in globular clusters or their strong time variability (see Fig. 2). We detected seven supernova remnants, one of which is a new candidate, and also ...
Accuracy of spectroscopy-based radioactive dating of stars
... sample of stars, and would as such be very valuable as a test of the theoretical stellar isochrones. Although potentially effective, spectroscopy-based radioactive dating is difficult to apply. The most easily measured longlived radioactive element, thorium, is only accessible (with the exception of st ...
... sample of stars, and would as such be very valuable as a test of the theoretical stellar isochrones. Although potentially effective, spectroscopy-based radioactive dating is difficult to apply. The most easily measured longlived radioactive element, thorium, is only accessible (with the exception of st ...
course objectives - Metropolitan Community College
... COURSE DESCRIPTION: This course is an introductory course in astronomy that covers the tools of astronomy, the night sky, the solar system, stars and star systems, galaxies, and cosmology. This is a lecture-only course. The lab course that complements this course is SCIE 1310. ...
... COURSE DESCRIPTION: This course is an introductory course in astronomy that covers the tools of astronomy, the night sky, the solar system, stars and star systems, galaxies, and cosmology. This is a lecture-only course. The lab course that complements this course is SCIE 1310. ...
Towards the understanding of the deepest layers of solar
... With the recent launch of the Kepler satellite, thousands of stars are being monitored to provide high-quality seismic data. These seismic data combined with non-seismic surface stellar observables can provide valuable information about the global properties of pulsating stars, such as their mass, r ...
... With the recent launch of the Kepler satellite, thousands of stars are being monitored to provide high-quality seismic data. These seismic data combined with non-seismic surface stellar observables can provide valuable information about the global properties of pulsating stars, such as their mass, r ...
flyer
... But, given the huge moment of inertia that the stars possess, this still represents a very large loss in rotational energy, corresponding to a power of ∼1031 Watts, or well over ten thousand times the Sun's luminosity. If we assume that all of this energy is being lost by emission of gravitational ...
... But, given the huge moment of inertia that the stars possess, this still represents a very large loss in rotational energy, corresponding to a power of ∼1031 Watts, or well over ten thousand times the Sun's luminosity. If we assume that all of this energy is being lost by emission of gravitational ...
the PDF program book
... There are five meeting rooms in UKK (rooms K1 – K4, K6) that may be used for meetings or telecons. The rooms are located on level 3 and seat between 12 and 24 people. If you want to hold a small meeting, you can either speak to the LOC representative at the registration desk or reserve a meeting roo ...
... There are five meeting rooms in UKK (rooms K1 – K4, K6) that may be used for meetings or telecons. The rooms are located on level 3 and seat between 12 and 24 people. If you want to hold a small meeting, you can either speak to the LOC representative at the registration desk or reserve a meeting roo ...
Starspots: A Key to the Stellar Dynamo | SpringerLink
... Thus, red dwarf stars are cooler, smaller, and less massive than the Sun. Correspondingly their luminosities range from 0.1% to about 8% of the solar luminosity. They constitute, at least, 80% of the stellar population in the Galaxy. Remarkable magnetic activity expressed in extremely strong optical ...
... Thus, red dwarf stars are cooler, smaller, and less massive than the Sun. Correspondingly their luminosities range from 0.1% to about 8% of the solar luminosity. They constitute, at least, 80% of the stellar population in the Galaxy. Remarkable magnetic activity expressed in extremely strong optical ...
The Time of Perihelion Passage and the Longitude of Perihelion of
... If Nemesis, a hypothetical solar companion star, periodically passes through the asteroid belt, it should have perturbed the orbits of the planets substantially, especially near times of perihelion passage. Yet almost no such perturbations have been detected. This can be explained if Nemesis is comp ...
... If Nemesis, a hypothetical solar companion star, periodically passes through the asteroid belt, it should have perturbed the orbits of the planets substantially, especially near times of perihelion passage. Yet almost no such perturbations have been detected. This can be explained if Nemesis is comp ...