Planetary detection limits taking into account stellar noise
... evolutionary stages, from subgiant to dwarf stars. Since data span between 5 and 8 days, only stellar noise sources with timescales shorter than this time span will be extracted from these observations. Therefore, we are able to study oscillation modes and granulation phenomena without being signifi ...
... evolutionary stages, from subgiant to dwarf stars. Since data span between 5 and 8 days, only stellar noise sources with timescales shorter than this time span will be extracted from these observations. Therefore, we are able to study oscillation modes and granulation phenomena without being signifi ...
Variability of solar/stellar activity and magnetic field and its influence... planetary atmosphere evolution
... plasma environment and solar/stellar magnetic field derived from the observations of solar proxies with different ages will be given. We show that the extreme radiation and plasma environments of the young Sun/stars have important implications for the evolution of planetary atmospheres and may be re ...
... plasma environment and solar/stellar magnetic field derived from the observations of solar proxies with different ages will be given. We show that the extreme radiation and plasma environments of the young Sun/stars have important implications for the evolution of planetary atmospheres and may be re ...
Detection of Organic Pollutants with a Pulsed Ion Mobility
... produces free electrons continuously and thus the ionization is a continuous process, devices operating with such sources are called to work in a continuous mode. Our device uses a novel electron gun that can be operated in pulsed mode, i.e. the electrons are emitted in short pulses with a certain d ...
... produces free electrons continuously and thus the ionization is a continuous process, devices operating with such sources are called to work in a continuous mode. Our device uses a novel electron gun that can be operated in pulsed mode, i.e. the electrons are emitted in short pulses with a certain d ...
~ ) Pergamon
... unit. The signal-to-noise ratio of the sampled analog signal is thus improved by reducing the sensitivity to changes in the ambient light level. The signal filtering electronic unit is tuned to the chopping frequency. The light is then collimated by a fixed 33 mm focal length quartz lens and polariz ...
... unit. The signal-to-noise ratio of the sampled analog signal is thus improved by reducing the sensitivity to changes in the ambient light level. The signal filtering electronic unit is tuned to the chopping frequency. The light is then collimated by a fixed 33 mm focal length quartz lens and polariz ...
Circumstellar medium around rotating massive stars at solar metallicity
... The second new tool is an elaborate, object-oriented implementation of the description of time-dependent stellar boundary conditions for entire stellar systems. For the present study, it allows us to accommodate in an easy and transparent way the timedependent boundary conditions of our single star. ...
... The second new tool is an elaborate, object-oriented implementation of the description of time-dependent stellar boundary conditions for entire stellar systems. For the present study, it allows us to accommodate in an easy and transparent way the timedependent boundary conditions of our single star. ...
Introduction The acronym LASER, which stands for light
... particle can also lose energy non-radiatively, in which case the energy is dissipated into heating. Atomic systems have only electronic states, which in the simple Bohr model of the atom correspond to different configurations of electron orbits. The types of energy state that exist in a molecular sy ...
... particle can also lose energy non-radiatively, in which case the energy is dissipated into heating. Atomic systems have only electronic states, which in the simple Bohr model of the atom correspond to different configurations of electron orbits. The types of energy state that exist in a molecular sy ...
GALAXIES 626
... Kinematics and structure of the thick disk rotational lag ~ 30 km/s near the sun and increases by about 30 km s-1 kpc-1 with height above the plane velocity dispersion in (U,V,W) = (46, 50, 35) km/s radial scale length = 3.5 to 4.5 kpc : uncertain scale height from star counts = 800 to 1200 pc (thi ...
... Kinematics and structure of the thick disk rotational lag ~ 30 km/s near the sun and increases by about 30 km s-1 kpc-1 with height above the plane velocity dispersion in (U,V,W) = (46, 50, 35) km/s radial scale length = 3.5 to 4.5 kpc : uncertain scale height from star counts = 800 to 1200 pc (thi ...
A Study of the Nature and Representative Features of Supernova
... The nature of supernovae was not initially understood. They were referred to as “guest stars” and seen as omens in a variety of cultures in Asian and European countries. Approximately 231 confirmed nearby (Galactic) supernovae remnants exist, with a few dozen other heavily suspected. For a listing a ...
... The nature of supernovae was not initially understood. They were referred to as “guest stars” and seen as omens in a variety of cultures in Asian and European countries. Approximately 231 confirmed nearby (Galactic) supernovae remnants exist, with a few dozen other heavily suspected. For a listing a ...
THE ABSOLUTE MAGNITUDE OF RR LYRAE - Cosmos
... stars with larger relative errors have brighter luminosities, i.e., have smaller parallaxes, appears clearly when the true parallax is small, compared with error of parallax. Similarly the distant stars have too faint luminosities, i.e., have too large parallaxes, mainly because the true parallax is ...
... stars with larger relative errors have brighter luminosities, i.e., have smaller parallaxes, appears clearly when the true parallax is small, compared with error of parallax. Similarly the distant stars have too faint luminosities, i.e., have too large parallaxes, mainly because the true parallax is ...
Dispersion and Ultrashort Pulses
... k”L is the 2nd-order spectral phase of the medium, then the resulting pulse 2nd-order phase will be the sum: 2 + k”L. A linearly chirped input pulse has 2nd-order phase: 2,in Emerging from a medium, its 2nd-order phase will be: ...
... k”L is the 2nd-order spectral phase of the medium, then the resulting pulse 2nd-order phase will be the sum: 2 + k”L. A linearly chirped input pulse has 2nd-order phase: 2,in Emerging from a medium, its 2nd-order phase will be: ...
A SIGNIFICANTLY LOW CO ABUNDANCE TOWARD THE TW Hya
... (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the reduced measured χ (CO) in the gas-phase is unlikely to be the result of freeze-out. In fact a number of studies ...
... (Aikawa et al. 1996; Dartois et al. 2003). Under normal conditions CO freezes-out at low temperatures present in the midplane, T 20 K, where HD does not strongly emit, and therefore the reduced measured χ (CO) in the gas-phase is unlikely to be the result of freeze-out. In fact a number of studies ...
CW9_MOST_GSphot_RK_v1
... MOST Guide Star Photometry • typically 4-8 guide stars, in special cases up to 20 are monitored for any given primary target • the magnitude range is 7-10.5, about 80% are of ‘known’ (listed) spectral type • exposure time is usually 1.5 sec (range from 0.3 to 1.5 applied) • no images are recovered, ...
... MOST Guide Star Photometry • typically 4-8 guide stars, in special cases up to 20 are monitored for any given primary target • the magnitude range is 7-10.5, about 80% are of ‘known’ (listed) spectral type • exposure time is usually 1.5 sec (range from 0.3 to 1.5 applied) • no images are recovered, ...
Magnetic Doppler imaging of the roAp star HD 24712⋆
... progressively increasing from one element to another and within different groups of lines of the same element. We propose that this pulsational behaviour is caused by the fact that these elements are concentrated in a thin layer in the stellar atmosphere where pulsation reaches its maximum amplitude ...
... progressively increasing from one element to another and within different groups of lines of the same element. We propose that this pulsational behaviour is caused by the fact that these elements are concentrated in a thin layer in the stellar atmosphere where pulsation reaches its maximum amplitude ...
HOLO TEXT
... Geometrical optics - this area of optics operates on the primary assumption that light travels in a straight line. Although this is an abstraction of reality, it nevertheless permits rather direct and accurate explanation and prediction of certain optical phenomena such as the focusing of light by l ...
... Geometrical optics - this area of optics operates on the primary assumption that light travels in a straight line. Although this is an abstraction of reality, it nevertheless permits rather direct and accurate explanation and prediction of certain optical phenomena such as the focusing of light by l ...
Astro 102 Practice Test 3
... c. indicates that the sun's core is much hotter than expected. d. indicates the sun's core is convective. e. none of the above 6. The carbon-nitrogen-oxygen cycle a. operates at a slightly lower temperature than the proton-proton chain. b. is most efficient in a star less massive than the sun. c. oc ...
... c. indicates that the sun's core is much hotter than expected. d. indicates the sun's core is convective. e. none of the above 6. The carbon-nitrogen-oxygen cycle a. operates at a slightly lower temperature than the proton-proton chain. b. is most efficient in a star less massive than the sun. c. oc ...
Influence of Protonation State on the Excited State Dynamics of a
... of Ru in the visible spectral range, were mainly associated with the pyrene moiety. 3.2. Femtosecond Transient Absorption Spectroscopy. After having discussed the ground-state absorption properties of the complex in its individual protonation states, we now shift the focus to the pH-dependent photoi ...
... of Ru in the visible spectral range, were mainly associated with the pyrene moiety. 3.2. Femtosecond Transient Absorption Spectroscopy. After having discussed the ground-state absorption properties of the complex in its individual protonation states, we now shift the focus to the pH-dependent photoi ...
Chapter two_part B
... Intrinsic Absorption: Caused by interaction with one or more of the components of the glass. ...
... Intrinsic Absorption: Caused by interaction with one or more of the components of the glass. ...
A Collection of Curricula for the STARLAB Polynesian Voyaging
... The kahako, the little dash over a vowel, denotes a stressed vowel sound. The ‘okina (‘), or glottal stop, signals a halting of breath before a vowel. Many centuries ago people looked up at the sky at night and thought that groups of stars formed figures. To these figures they gave names to honor ch ...
... The kahako, the little dash over a vowel, denotes a stressed vowel sound. The ‘okina (‘), or glottal stop, signals a halting of breath before a vowel. Many centuries ago people looked up at the sky at night and thought that groups of stars formed figures. To these figures they gave names to honor ch ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.