Towards the understanding of the deepest layers of solar
... I would like to start by thanking both my supervisors, Dra. Margarida Cunha and Prof. Dr. Jørgen Christensen-Dalsgaard, without whom the realization of this thesis would not have been possible. I would like to give a very special thank to Prof. Dr. Jørgen ChristensenDalsgaard for his hospitality and ...
... I would like to start by thanking both my supervisors, Dra. Margarida Cunha and Prof. Dr. Jørgen Christensen-Dalsgaard, without whom the realization of this thesis would not have been possible. I would like to give a very special thank to Prof. Dr. Jørgen ChristensenDalsgaard for his hospitality and ...
ASI 2017 Abstract Book - Astronomical Society of India
... Rengaswamy Sridharan - Imaging with Masked Apertures: Application to Solar Imaging Parallel Session – Stars, ISM and the Galaxy – 1 Sarita Vig - An insight into massive star formation in dense cores of molecular clouds Blesson Mathew - The curious case of PDS 11: a nearby, >10 Myr old, classical T T ...
... Rengaswamy Sridharan - Imaging with Masked Apertures: Application to Solar Imaging Parallel Session – Stars, ISM and the Galaxy – 1 Sarita Vig - An insight into massive star formation in dense cores of molecular clouds Blesson Mathew - The curious case of PDS 11: a nearby, >10 Myr old, classical T T ...
Astronomy 113 Laboratory Manual - UW
... Polaris, the North Star, has long shown the way to travelers. At sea the only "landmarks" are celestial. It was Polaris that guided sailors around the globe, and not only by showing the way North. Using a sextant a European captain sailing to the New World could also accurately find the ship's latit ...
... Polaris, the North Star, has long shown the way to travelers. At sea the only "landmarks" are celestial. It was Polaris that guided sailors around the globe, and not only by showing the way North. Using a sextant a European captain sailing to the New World could also accurately find the ship's latit ...
Chapter 5 The Evolutionary Paths Of Nearby Galaxies
... misclassified or peculiar objects and their properties will be investigated later. To investigate whether the quenching is due to AGN feedback or environmental effects, I divide the sample according to nuclear activity and Hi content (Figure 5.1, top row, central and right panel, respectively), as d ...
... misclassified or peculiar objects and their properties will be investigated later. To investigate whether the quenching is due to AGN feedback or environmental effects, I divide the sample according to nuclear activity and Hi content (Figure 5.1, top row, central and right panel, respectively), as d ...
DUSTiNGS III: Distribution of Intermediate
... radial profiles, these studies report the presence of both intermediate-age and older populations in the outer regions of a sub-sample of the galaxies studied. In this study, we selected the nine nearby dwarf galaxies that host > 90% of the identified variable AGB star candidates from the larger DUS ...
... radial profiles, these studies report the presence of both intermediate-age and older populations in the outer regions of a sub-sample of the galaxies studied. In this study, we selected the nine nearby dwarf galaxies that host > 90% of the identified variable AGB star candidates from the larger DUS ...
ROSAT Ian R. Stevens* and David K. Strickland*
... spectra with typically kT , 0:4¹1:0 keV. There are some oddities: NGC 5408 is very overluminous in X-rays, even compared with other WR galaxies; I Zw 18 has a harder Xray spectrum; NGC 1365, although thought to contain an active nucleus, has X-ray properties that are broadly similar to other WR gala ...
... spectra with typically kT , 0:4¹1:0 keV. There are some oddities: NGC 5408 is very overluminous in X-rays, even compared with other WR galaxies; I Zw 18 has a harder Xray spectrum; NGC 1365, although thought to contain an active nucleus, has X-ray properties that are broadly similar to other WR gala ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
... The OGLE-III data reveal an O-rich star in the SMC with a period of 1749 days. Its absolute magnitude of Mbol = −8.0 makes it a good candidate for a super-AGB star. Key words. stars: AGB and post-AGB – stars: mass loss – Magellanic Clouds ...
The spectroscopic Hertzsprung
... that the absolute brightnesses, i.e., the distances, are required to properly order the stars in the HR diagram. Order can also be achieved for stars in star clusters where the distance may still be unknown, but the distances of all stars are roughly equal, in what we now call color-magnitude diagra ...
... that the absolute brightnesses, i.e., the distances, are required to properly order the stars in the HR diagram. Order can also be achieved for stars in star clusters where the distance may still be unknown, but the distances of all stars are roughly equal, in what we now call color-magnitude diagra ...
Practical cosmology with the Local Volume galaxies
... i.e. obtain the known Schmidt-Kennicutt law (Kennicutt, 1998), but for the galaxies themselves, not for individual HII regions only. Therefore, evolutionary history of disks of galaxies looks to be driven mainly by internal SF processes. It is generally accepted that the enhanced star formation in g ...
... i.e. obtain the known Schmidt-Kennicutt law (Kennicutt, 1998), but for the galaxies themselves, not for individual HII regions only. Therefore, evolutionary history of disks of galaxies looks to be driven mainly by internal SF processes. It is generally accepted that the enhanced star formation in g ...
The Most Luminous Protostars in Molecular Clouds: A Hint to
... et al. 1998). The masses of the bright-rimmed clouds were estimated from their apparent sizes on the optical images and from a typical density for the clouds (n[H2 ] = 3 × 104 cm−3 ), as suggested by the authors (Sugitani et al. 1991). In one of our earlier studies toward the Cygnus region (Dobashi ...
... et al. 1998). The masses of the bright-rimmed clouds were estimated from their apparent sizes on the optical images and from a typical density for the clouds (n[H2 ] = 3 × 104 cm−3 ), as suggested by the authors (Sugitani et al. 1991). In one of our earlier studies toward the Cygnus region (Dobashi ...
3. Cosmology and the Origin and Evolution of Galaxies
... spectroscopic follow-up at mm wavelengths will place very strong constraints on the evolutionary history of star formation in this important galaxy population, and challenge the currently accepted scenarios for massive-galaxy formation. ...
... spectroscopic follow-up at mm wavelengths will place very strong constraints on the evolutionary history of star formation in this important galaxy population, and challenge the currently accepted scenarios for massive-galaxy formation. ...
Evolution of low mass stars
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
... The HRD inspired an English astronomer, Sir Arthur Stanley Eddington (18821944), when Russell visited London and presented his diagram at a meeting of the Royal Astronomical Society in 1913 (Eisberg, 2002). At the time, Eddington was the chief assistant of the Royal Greenwich Observatory. In 1926 Ed ...
Pdf - Text of NPTEL IIT Video Lectures
... considered that psi of x is equal to I consider this as a super position of plane waves under root of two pi h cross minus infinity a one dimensional wave packet a of p E to the power of i by h cross p x d p. Now the expectation value of p as we had discussed earlier is equal to psi star p psi where ...
... considered that psi of x is equal to I consider this as a super position of plane waves under root of two pi h cross minus infinity a one dimensional wave packet a of p E to the power of i by h cross p x d p. Now the expectation value of p as we had discussed earlier is equal to psi star p psi where ...
Lokal fulltext - Chalmers Publication Library
... in 1984 at Vega (α Lyrae, spectral class A0 V) by Aumann et al. (1984) with IRAS (Infrared Astronomical Satellite). However, as they saw the dust emission only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpre ...
... in 1984 at Vega (α Lyrae, spectral class A0 V) by Aumann et al. (1984) with IRAS (Infrared Astronomical Satellite). However, as they saw the dust emission only in the spectral energy distribution (SED) they could not infer any shape. The excess is beyond 12 µm and peaks close to 60 µm. They interpre ...
Chemical Evolution of Galactic Systems
... The chemical evolution code is first calibrated using empirical constraints from the Milky Way. These simulations help shed light on the nature of the gas accretion processes that fueled the formation of our Galaxy. We demonstrate the importance of low- and intermediate-mass stars in explaining the ...
... The chemical evolution code is first calibrated using empirical constraints from the Milky Way. These simulations help shed light on the nature of the gas accretion processes that fueled the formation of our Galaxy. We demonstrate the importance of low- and intermediate-mass stars in explaining the ...
LCM SerieS
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
... computer automated technology. Simple and friendly to use, the LCM telescope is up and running after locating just three bright celestial objects. It’s the perfect combination of power and portability. If you are new to astronomy, you may wish to start off by using the LCM’s built-in Sky Tour featur ...
maximum likelihood fitting of tidal streams with application
... There are two main tasks to implementing the maximum likelihood technique. The first is to develop the likelihood function, which measures the probability of observing a particular data set given a parameterized model. The second is to maximize the likelihood with respect to the parameters. In devel ...
... There are two main tasks to implementing the maximum likelihood technique. The first is to develop the likelihood function, which measures the probability of observing a particular data set given a parameterized model. The second is to maximize the likelihood with respect to the parameters. In devel ...
Radio pulsars
... • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
... • Young pulsars have unpredictable changes in period glitches and period noise. • Millisecond pulsars have extremely stable periods. ...
Jul y 9- 11,
... evidence for the termination of star formation at early epochs that drives some galaxies away from the “standard” correlation of stellar bulge mass with SMBH mass, and address how future X-ray missions can explore the evolution of hot coronae and SMBHs from z 6 to the present. ...
... evidence for the termination of star formation at early epochs that drives some galaxies away from the “standard” correlation of stellar bulge mass with SMBH mass, and address how future X-ray missions can explore the evolution of hot coronae and SMBHs from z 6 to the present. ...
The Evolution of Isotope Ratios in the Milky Way Galaxy
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
... metals are produced. This assumption may not be valid but does not affect the average chemical evolution of galaxies. Super AGB stars — The fate of stars with initial masses between about 8 − 10M⊙ is uncertain. The upper limit of AGB stars, Mu,1 , is defined as the minimum mass for carbon ignition, ...
A Spitzer mid-infrared spectral survey of mass
... Bessell & Fox 1983; Feast et al. 1989), and the intermediate-age clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright ox ...
... Bessell & Fox 1983; Feast et al. 1989), and the intermediate-age clusters NGC 419 and 1978, both of which have a known mid-IR source. Targets were selected to span the long sequence of increasing mass-loss in LIMS which stretches from (J − K , M K ) ∼ (2, − 9) to (7, −4) in Fig. 1(a). [The bright ox ...
Perseus (constellation)
Perseus, named after the Greek mythological hero Perseus, is a constellation in the northern sky. It was one of 48 listed by the 2nd-century astronomer Ptolemy and among the 88 modern constellations defined by the International Astronomical Union (IAU). It is located in the northern celestial hemisphere near several other constellations named after legends surrounding Perseus, including Andromeda to the west and Cassiopeia to the north. Perseus is also bordered by Aries and Taurus to the south, Auriga to the east, Camelopardalis to the north, and Triangulum to the west.The galactic plane of the Milky Way passes through Perseus but is mostly obscured by molecular clouds. The constellation's brightest star is the yellow-white supergiant Alpha Persei (also called Mirfak), which shines at magnitude 1.79. It and many of the surrounding stars are members of an open cluster known as the Alpha Persei Cluster. The best-known star, however, is Algol (Beta Persei), linked with ominous legends because of its variability, which is noticeable to the naked eye. Rather than being an intrinsically variable star, it is an eclipsing binary. Other notable star systems in Perseus include X Persei, a binary system containing a neutron star, and GK Persei, a nova that peaked at magnitude 0.2 in 1901. The Double Cluster, comprising two open clusters quite near each other in the sky, was known to the ancient Chinese. The constellation gives its name to the Perseus Cluster (Abell 426), a massive galaxy cluster located 250 million light-years from Earth. It hosts the radiant of the annual Perseids meteor shower—one of the most prominent meteor showers in the sky.