Fulltext PDF - Indian Academy of Sciences
... on the kinds of speeds one encounters in the world around. We can see a centipede crawling at a few centimeters in ten seconds, a fast walker can cover a few kilometers in an hour, but jaguars dart at more than a hundred. Racing cars zoom at a few hundred kilometers an hour, while jet planes travel ...
... on the kinds of speeds one encounters in the world around. We can see a centipede crawling at a few centimeters in ten seconds, a fast walker can cover a few kilometers in an hour, but jaguars dart at more than a hundred. Racing cars zoom at a few hundred kilometers an hour, while jet planes travel ...
Sardinia_SA - Mullard Space Science Laboratory
... • Many systems show strong variability due to flaring on timescales of tens of seconds • Some systems show quasiperiodic oscillations on a timescale of seconds: this is due to an intrinsic instability in the cooling gas accreting onto the white dwarf ...
... • Many systems show strong variability due to flaring on timescales of tens of seconds • Some systems show quasiperiodic oscillations on a timescale of seconds: this is due to an intrinsic instability in the cooling gas accreting onto the white dwarf ...
... the hottest [WC] stars (Keller et al. 2014), showing a wide range in the C/He ratio, high Ne abundances, and N abundances much higher than those found in previous determinations. Six new emission line stars were discovered by Górny (2014), including two [WC] stars and one VL (or [WC11]) star, makin ...
Living in the Milky Way - The Cupola: Scholarship at Gettysburg
... ponder what you’re seeing: our own home galaxy, made up of over 100 billion stars and other material, viewed from the inside. The you see light is the accumulated glow of a small fraction of those faint stars. The Milky Way, as a giant spiral galaxy, is fairly flat (only 2,000 light years thick but ...
... ponder what you’re seeing: our own home galaxy, made up of over 100 billion stars and other material, viewed from the inside. The you see light is the accumulated glow of a small fraction of those faint stars. The Milky Way, as a giant spiral galaxy, is fairly flat (only 2,000 light years thick but ...
may10-94 as a Word 6.0 doc - Lyle School of Engineering
... 4) The last three pages of this exam contain supplementary figures and information that may be useful in solving some of the problems below. ...
... 4) The last three pages of this exam contain supplementary figures and information that may be useful in solving some of the problems below. ...
Extragalactic Astronomical Masers I
... Maser (Microwave Amplification by Stimulated Emission of Radiation) is a radio wave equivalent of laser at optical wavelength. Laser is an acronym for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser ligh ...
... Maser (Microwave Amplification by Stimulated Emission of Radiation) is a radio wave equivalent of laser at optical wavelength. Laser is an acronym for Light Amplification by Stimulated Emission of Radiation. Laser is an artificial light and it is very different from other lights in that a laser ligh ...
Laser Modes
... atoms to radiate photons into the same state, thus forming a phase coherent and parallel beam. Thus, a standing wave develops between the two mirrors at either end of the cavity. The allowed wavelengths are those for which the cavity length is an integral number of half wavelengths. Photons are not ...
... atoms to radiate photons into the same state, thus forming a phase coherent and parallel beam. Thus, a standing wave develops between the two mirrors at either end of the cavity. The allowed wavelengths are those for which the cavity length is an integral number of half wavelengths. Photons are not ...
General Module information
... – the physical effects leading to the red giant branch Qualitatively explain how the evolution of low mass stars differ from the above. Explain qualitatively how the post-RGB evolution of low mass stars leads to the formation of planetary nebulas and white dwarfs. Explain how the asymptotic giant br ...
... – the physical effects leading to the red giant branch Qualitatively explain how the evolution of low mass stars differ from the above. Explain qualitatively how the post-RGB evolution of low mass stars leads to the formation of planetary nebulas and white dwarfs. Explain how the asymptotic giant br ...
looking for progenitors of cool Ap stars
... Recently, we have studied the evolutionary state of magnetic Ap stars of mass below 3M using Hipparcos data (ESA 1997). We could show that the distribution of Ap stars in the H-R diagram differs from that of the normal stars in the same temperature range at a high level of significance (Hubrig et a ...
... Recently, we have studied the evolutionary state of magnetic Ap stars of mass below 3M using Hipparcos data (ESA 1997). We could show that the distribution of Ap stars in the H-R diagram differs from that of the normal stars in the same temperature range at a high level of significance (Hubrig et a ...
The Search for Exoplanets - Worcester Polytechnic Institute
... destruction of the Sassanid Persian state at the hands of the Arabs in the 630s, it is likely that the much praised astronomical knowledge of the Arab world had its beginnings from this golden age of Indian astronomy. As links between the East and West grew with the development of the Silk Road and ...
... destruction of the Sassanid Persian state at the hands of the Arabs in the 630s, it is likely that the much praised astronomical knowledge of the Arab world had its beginnings from this golden age of Indian astronomy. As links between the East and West grew with the development of the Silk Road and ...
Zhu Qualifier Solutions - University of Toronto Astronomy
... 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How do you determine an a present-day mass function (PDMF) from an IMF? 3 ...
... 3.1.3. Why are the lower and upper limits of the IMF poorly understood compared to that of the middle (several M stars)? What constraints are there? 3.1.4. What’s the difference between a field and stellar cluster IMF? 3.1.5. How do you determine an a present-day mass function (PDMF) from an IMF? 3 ...
Mass segregation in star clusters is not energy equipartition
... of lower-mass stars. We find that the most massive stars do not slow down faster than the average stars during mass segregation. In some ways this is not surprising; as the massive stars move towards the cluster centre, they fall deeper into the gravitational potential and would be expected to speed ...
... of lower-mass stars. We find that the most massive stars do not slow down faster than the average stars during mass segregation. In some ways this is not surprising; as the massive stars move towards the cluster centre, they fall deeper into the gravitational potential and would be expected to speed ...
end-of-summer report
... 11 years. He recognized more spectral transition lines than initially expected while analyzing the Sun. When an active region on the Sun was observed, he noticed his spectra had more absorption lines within a very small energy range where there is typically only one. This is known as Zeeman Splittin ...
... 11 years. He recognized more spectral transition lines than initially expected while analyzing the Sun. When an active region on the Sun was observed, he noticed his spectra had more absorption lines within a very small energy range where there is typically only one. This is known as Zeeman Splittin ...
The dramatic change of the fossil magnetic field of HD 190073
... broadening may be dominated by turbulence, and only slightly affected by rotation (Catala et al. 2007). As a consequence we may have only a limited access to the rotational Doppler resolution inside the spectral lines. This Doppler resolution is useful to study the polarisation level per rotational ...
... broadening may be dominated by turbulence, and only slightly affected by rotation (Catala et al. 2007). As a consequence we may have only a limited access to the rotational Doppler resolution inside the spectral lines. This Doppler resolution is useful to study the polarisation level per rotational ...
Black holes in binary systems and galatic nuclei
... Up to now from the borders of many special Xray space observatories (Einstein, Rosat, XMM Newton, Integral etc.) several thousands of Xray binaries have been discovered. Optical investigations made by many scientific groups (USA, England, Germany, Russia etc.) allowed to estimate the masses of 26 st ...
... Up to now from the borders of many special Xray space observatories (Einstein, Rosat, XMM Newton, Integral etc.) several thousands of Xray binaries have been discovered. Optical investigations made by many scientific groups (USA, England, Germany, Russia etc.) allowed to estimate the masses of 26 st ...
Giant molecular clouds in the dwarf galaxy NGC 1569
... dwarf starburst galaxy NGC 1569 with the IRAM interferometer on Plateau de Bure. We find the CO emission is not spatially associated with the two super star clusters in the galaxy, but rather is found in the vicinity of an HII region. With the resolution of our data, we can resolve the CO emission i ...
... dwarf starburst galaxy NGC 1569 with the IRAM interferometer on Plateau de Bure. We find the CO emission is not spatially associated with the two super star clusters in the galaxy, but rather is found in the vicinity of an HII region. With the resolution of our data, we can resolve the CO emission i ...
BARS FROM THE INSIDE OUT: AN HST STUDY OF THEIR DUSTY
... strength, while tightly wound dust spirals are only present in the most axisymmetric galaxies. In the subset of galaxies classified SB(s), SB(rs), or SB(r), GD structure is only found at the centers of SB(s) or SB(rs) galaxies, and not SB(r). Bar strength measurements of 35 SB(s), SB(rs), and SB(r) ...
... strength, while tightly wound dust spirals are only present in the most axisymmetric galaxies. In the subset of galaxies classified SB(s), SB(rs), or SB(r), GD structure is only found at the centers of SB(s) or SB(rs) galaxies, and not SB(r). Bar strength measurements of 35 SB(s), SB(rs), and SB(r) ...
Pulsation spectrum of δ Scuti stars: the binary HD 50870 as seen
... automated f77 code, which also allows detecting more frequencies (Period04 is limited to about 200 components). The frequency analysis was performed using the relative fluxes, then the results were scaled into mmag units. We detected 734 frequencies with amplitudes ranging from 12.961 mmag down to 0 ...
... automated f77 code, which also allows detecting more frequencies (Period04 is limited to about 200 components). The frequency analysis was performed using the relative fluxes, then the results were scaled into mmag units. We detected 734 frequencies with amplitudes ranging from 12.961 mmag down to 0 ...
Document
... based telescopes can now reach their theoretical resolution limit. Hence 8 meter AO equipped telescopes (like Gemini) can read a license plate 20 miles away (this is 20 times farther than without AO). For astronomical science adaptive optics has made the sharpest, clearest images of: ...
... based telescopes can now reach their theoretical resolution limit. Hence 8 meter AO equipped telescopes (like Gemini) can read a license plate 20 miles away (this is 20 times farther than without AO). For astronomical science adaptive optics has made the sharpest, clearest images of: ...
Main-Sequence Stars and the Sun
... 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 state, therefore the Balmer lines are weak. As the temperature inc ...
... 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 state, therefore the Balmer lines are weak. As the temperature inc ...
Discovery probability of transiting extragalactic planets and
... In the first section of this diploma, we present the first statistical analysis on extra galactic stars that could host an exoplanet. We analyze the photometric data of the Ursa Minor Dwarf (UMi Dwarf) spheroidal galaxy, taken with the 2.5 m Isaac Newton Group Telescope (INT) and we calculate the pr ...
... In the first section of this diploma, we present the first statistical analysis on extra galactic stars that could host an exoplanet. We analyze the photometric data of the Ursa Minor Dwarf (UMi Dwarf) spheroidal galaxy, taken with the 2.5 m Isaac Newton Group Telescope (INT) and we calculate the pr ...
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.