Introduction_to_pulsar_astronomy
... Radio scintillation studies led Hewish and Okoye (1964) to propose the existence of a compact radio source near the center of the nebula, with a steep spectrum. Pacini (1967) proposed the existence of a highly magnetized, rapidly spinning neutron star as the power source of the nebula. This would ra ...
... Radio scintillation studies led Hewish and Okoye (1964) to propose the existence of a compact radio source near the center of the nebula, with a steep spectrum. Pacini (1967) proposed the existence of a highly magnetized, rapidly spinning neutron star as the power source of the nebula. This would ra ...
azu_etd_13224_sip1_m
... Within the last 20 years, and particularly during the time I have been in graduate school, the search for and discovery of planets outside of our Solar System has accelerated dramatically, exposing the great diversity in the outcomes of planet formation and evolution within our Galaxy. The raw mater ...
... Within the last 20 years, and particularly during the time I have been in graduate school, the search for and discovery of planets outside of our Solar System has accelerated dramatically, exposing the great diversity in the outcomes of planet formation and evolution within our Galaxy. The raw mater ...
Review: How does a star`s mass determine its life story?
... • size R ~ thousands of kilometers • mass M ~ mass of stars • density absurdly high: – white dwarf matter is roughly a million times more dense than water atomic density ...
... • size R ~ thousands of kilometers • mass M ~ mass of stars • density absurdly high: – white dwarf matter is roughly a million times more dense than water atomic density ...
PP Chapter 28 Text
... Life cycle of stars: • Begins as a nebula • Advances to a protostar • Becomes a star when fusion in its core occurs Depending on its mass, the star may become a red giant and then burn out to become a white dwarf. ...
... Life cycle of stars: • Begins as a nebula • Advances to a protostar • Becomes a star when fusion in its core occurs Depending on its mass, the star may become a red giant and then burn out to become a white dwarf. ...
The Most Luminous Protostars in Molecular Clouds: A Hint to
... regions. Actually, the two methods (LTE and virial) yield consistent values mostly within a factor of < 2 for GMCs in the outer arm (Mead, Kutner 1988). We therefore conclude that the cloud masses which we gathered from the literature should be consistent within a small factor. However, errors in th ...
... regions. Actually, the two methods (LTE and virial) yield consistent values mostly within a factor of < 2 for GMCs in the outer arm (Mead, Kutner 1988). We therefore conclude that the cloud masses which we gathered from the literature should be consistent within a small factor. However, errors in th ...
A Determination of the Deflection of Light by the Sun`s Gravitational
... the third alternative, and confirmEINSTEIN'Sgeneralisedrelativity theory. As is wellknown the theory is also confirmedby the lotion of the perihelion of ATercury,which exceeds the Newtonian value by 43" per century-an amount practically identical with that deduced from EINSTEIN'Stheory. 0n the other ...
... the third alternative, and confirmEINSTEIN'Sgeneralisedrelativity theory. As is wellknown the theory is also confirmedby the lotion of the perihelion of ATercury,which exceeds the Newtonian value by 43" per century-an amount practically identical with that deduced from EINSTEIN'Stheory. 0n the other ...
Program and Abstract Book - European Southern Observatory
... condense into higher density clumps to form individual stars or stellar clusters. The study of the kinematics of the filaments through single-dish observations suggests the presence of gas flows along the filaments, oscillatory motions due to gravity infall, and the existence of substructure inside ...
... condense into higher density clumps to form individual stars or stellar clusters. The study of the kinematics of the filaments through single-dish observations suggests the presence of gas flows along the filaments, oscillatory motions due to gravity infall, and the existence of substructure inside ...
Annual Report 2006/2007
... Stars form in galaxies from interstellar material, and at the end of their lives return chemicallyenriched material to the interstellar medium from which new generations of stars and planets form. The most massive and luminous stars evolve fastest, and leave neutron stars and black holes. This life ...
... Stars form in galaxies from interstellar material, and at the end of their lives return chemicallyenriched material to the interstellar medium from which new generations of stars and planets form. The most massive and luminous stars evolve fastest, and leave neutron stars and black holes. This life ...
A Search for Extrasolar Planets Using Echoes Produced in Flare
... the other to the nearby object where the pulse is then reflected to the observer. In this model, the nearby object would be detected as a secondary pulse with amplitude decreased and at a time delay ∆t. The amplitude reduction comes from the reflectivity and relative size of the object while the tim ...
... the other to the nearby object where the pulse is then reflected to the observer. In this model, the nearby object would be detected as a secondary pulse with amplitude decreased and at a time delay ∆t. The amplitude reduction comes from the reflectivity and relative size of the object while the tim ...
Trapezium Fracture
... glimpsing a vision of our own Sun and solar system’s creation 4.5 billion years ago. Current theory holds that our own Solar system was created out of a similar massive nebula. Within M42 are thousands of protostars and young stars, less than one million years old. Will one of these stars in a far d ...
... glimpsing a vision of our own Sun and solar system’s creation 4.5 billion years ago. Current theory holds that our own Solar system was created out of a similar massive nebula. Within M42 are thousands of protostars and young stars, less than one million years old. Will one of these stars in a far d ...
Galaxy Sorting
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
... galaxies contain mostly old stars, with very little gas and dust found between stars. Since new stars form from clouds of interstellar gas and dust, elliptical galaxies lack the raw ingredients to make new stars. Spiral galaxies, on the other hand, have a mix of young and old stars. Interstellar ...
Spot sizes on Sun-like stars
... This is described in more detail later. The measurements of the photometric spot coverages (column 6 in Table 2) are taken from Henry et al. (1995), Rodonò et al. (2000) and Padmakar & Pandey (1999) and are labelled H+, R+ and PP, respectively, in column 7. The covering fractions derived from photo ...
... This is described in more detail later. The measurements of the photometric spot coverages (column 6 in Table 2) are taken from Henry et al. (1995), Rodonò et al. (2000) and Padmakar & Pandey (1999) and are labelled H+, R+ and PP, respectively, in column 7. The covering fractions derived from photo ...
Improved stellar parameters of CoRoT-7
... agreement with the adjacent order is very good and there is acWe used the VWA package (Bruntt et al. 2004, 2008; Bruntt ceptable agreement with the template. The overlapping orders 2009) to analyse the spectra listed in Table 1. It can perform are finally merged to improve the S/N by up to 40%. When ...
... agreement with the adjacent order is very good and there is acWe used the VWA package (Bruntt et al. 2004, 2008; Bruntt ceptable agreement with the template. The overlapping orders 2009) to analyse the spectra listed in Table 1. It can perform are finally merged to improve the S/N by up to 40%. When ...
Variations in Integrated Galactic Initial Mass Functions due to
... 2006, the latter WK06 from now on) pointed out that the distribution of initial stellar masses in a galaxy may significantly deviate from the initial mass function (IMF) the stars have when they are born, if the vast majority of stars is born in clusters. These clusters follow a power-law mass funct ...
... 2006, the latter WK06 from now on) pointed out that the distribution of initial stellar masses in a galaxy may significantly deviate from the initial mass function (IMF) the stars have when they are born, if the vast majority of stars is born in clusters. These clusters follow a power-law mass funct ...
Galactic Stellar and Substellar Initial Mass Function Invited Review Gilles Chabrier
... power-law approximations, dN/dm ∝ m!a, as initially suggested by Salpeter (1955), with an exponent close to the Salpeter value a p 2.35. A departure from this monotonic behavior, with a flattening of the MF below ∼1 M,, was first proposed by MS79, who suggested a lognormal form. The tremendous progr ...
... power-law approximations, dN/dm ∝ m!a, as initially suggested by Salpeter (1955), with an exponent close to the Salpeter value a p 2.35. A departure from this monotonic behavior, with a flattening of the MF below ∼1 M,, was first proposed by MS79, who suggested a lognormal form. The tremendous progr ...
Plotting the Rotation Curve of M31
... In this activity students use real data, taken from a scientific paper, to plot the rotational curve of M31 (Andromeda), our neighbouring spiral galaxy. They will look at Kepler’s third law to predict the motion of stars around the centre of M31. They will then measure the wavelengths of hydrogen emi ...
... In this activity students use real data, taken from a scientific paper, to plot the rotational curve of M31 (Andromeda), our neighbouring spiral galaxy. They will look at Kepler’s third law to predict the motion of stars around the centre of M31. They will then measure the wavelengths of hydrogen emi ...
On the interpretation of stellar disc observations in terms of diameters
... Key words: methods: miscellaneous ± stars: fundamental parameters ± stars: general. ...
... Key words: methods: miscellaneous ± stars: fundamental parameters ± stars: general. ...
White dwarf binary
... Stellar death Supernova remnant Role of Mass White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binarie ...
... Stellar death Supernova remnant Role of Mass White dwarfs White dwarf limit White dwarf binary Accretion disks Thought question Nova Thought question 2 types of SN Nova or supernova? Standard candles Neutron stars Discovery Crab pulsar Pulsars Pulsars are NS! Magnetic fields Thought question Binarie ...
Towards the understanding of the deepest layers of solar
... 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 unconditional support during my three month working visit at Aarhus University. Although ...
... 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 unconditional support during my three month working visit at Aarhus University. Although ...
Stellar kinematics
Stellar kinematics is the study of the movement of stars without needing to understand how they acquired their motion. This differs from stellar dynamics, which takes into account gravitational effects. The motion of a star relative to the Sun can provide useful information about the origin and age of a star, as well as the structure and evolution of the surrounding part of the Milky Way.In astronomy, it is widely accepted that most stars are born within molecular clouds known as stellar nurseries. The stars formed within such a cloud compose open clusters containing dozens to thousands of members. These clusters dissociate over time. Stars that separate themselves from the cluster's core are designated as members of the cluster's stellar association. If the remnant later drifts through the Milky Way as a coherent assemblage, then it is termed a moving group.