Planet formation around stars of various masses: The snow line and
... Ida & Lin (2005) examined observable planetary systems resulting from type II migration. Kornet et al. consider disk evolution prior to the growth of large objects. In their models, the increased inward migration rate for planetesimals around low-mass stars results in higher absolute surface densiti ...
... Ida & Lin (2005) examined observable planetary systems resulting from type II migration. Kornet et al. consider disk evolution prior to the growth of large objects. In their models, the increased inward migration rate for planetesimals around low-mass stars results in higher absolute surface densiti ...
the Colours of rainbow the Brook
... c. Irregular galaxies:Theses galaxies do not have any particular shape and are only 2% of the total normal galaxy. They are the youngest galaxies in the universe. Radio galaxies:Those galaxies which emit radiations in radio wave range are called radio galaxies. They are identified by using radio te ...
... c. Irregular galaxies:Theses galaxies do not have any particular shape and are only 2% of the total normal galaxy. They are the youngest galaxies in the universe. Radio galaxies:Those galaxies which emit radiations in radio wave range are called radio galaxies. They are identified by using radio te ...
The Physics of Star Formation: Understanding the Youngest Protostars
... over 5 m < < 30 m as a thick curve. Most known Class 0 YSOs are equally or somewhat less luminous and approximately a factor of 3 more distant. Thus they are about a factor of 10 fainter but should still be observable (continua at R > 5 and lines at R > 1000). ...
... over 5 m < < 30 m as a thick curve. Most known Class 0 YSOs are equally or somewhat less luminous and approximately a factor of 3 more distant. Thus they are about a factor of 10 fainter but should still be observable (continua at R > 5 and lines at R > 1000). ...
Protostellar/PMS Mass Infall Luminosity Problem
... luminosity). Now that more massive protostars are included, the match with our PLF is much improved. ...
... luminosity). Now that more massive protostars are included, the match with our PLF is much improved. ...
17_Testbank
... 4) There is no limit to the mass with which a star can be born. Answer: FALSE 5) Stars with high masses live longer than stars with lower masses. Answer: FALSE 6) Stars of lower mass have deeper convection zones outside their cores than stars of higher mass. Answer: TRUE 7) Convection never occurs i ...
... 4) There is no limit to the mass with which a star can be born. Answer: FALSE 5) Stars with high masses live longer than stars with lower masses. Answer: FALSE 6) Stars of lower mass have deeper convection zones outside their cores than stars of higher mass. Answer: TRUE 7) Convection never occurs i ...
Absolute magnitudes and kinematics of barium
... analysed in order to assess a possible evolutionary link between the groups. We have used the kinematical results in order to estimate an average sample age for each group from the age-dispersion relationship given by Lacey (1992). The total velocity dispersions have been evaluated from the data of ...
... analysed in order to assess a possible evolutionary link between the groups. We have used the kinematical results in order to estimate an average sample age for each group from the age-dispersion relationship given by Lacey (1992). The total velocity dispersions have been evaluated from the data of ...
Final Exam Review
... a. 10.0 degrees Celsius and a pressure of 218 atmospheres b. slightly warmer than 0.0 degrees Celsius and a pressure of 0.33 atmosphere c. 150 degrees Celsius and a pressure of 180 atmospheres d. 200 degrees Celsius and a pressure of 150 atmospheres ____ 44. Based on the information in the phase dia ...
... a. 10.0 degrees Celsius and a pressure of 218 atmospheres b. slightly warmer than 0.0 degrees Celsius and a pressure of 0.33 atmosphere c. 150 degrees Celsius and a pressure of 180 atmospheres d. 200 degrees Celsius and a pressure of 150 atmospheres ____ 44. Based on the information in the phase dia ...
6.1 Introduction
... relies on spectroscopic observations. The absorption lines formed in the atmospheres of stars contain a wealth of information, on the temperature, gravity, rotational velocity and chemical composition of the star. The last one in particular is of great interest as it reflects (for stars on the main ...
... relies on spectroscopic observations. The absorption lines formed in the atmospheres of stars contain a wealth of information, on the temperature, gravity, rotational velocity and chemical composition of the star. The last one in particular is of great interest as it reflects (for stars on the main ...
P7 Further Physics
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
... Astronomers often use the “parsec” to describe galactic distances. A parsec is roughly 3¼ light years. Angles involved in parallax measurements are often very small and are measured in seconds of an arc (arcseconds). A second of an arc is 1/60th of a minute of an arc, which is 1/60th of a degree. In ...
Astronomical Picture of the Day
... The Orion Nebula (a) is a giant cloud of gas and dust in which new stars and planets are forming. It is located about 1,500 light-years from Earth, which means the light recorded in the photograph took about 1,500 years to reach us. Thus, we see it as it was about 1,500 years ago. Photograph (b) sho ...
... The Orion Nebula (a) is a giant cloud of gas and dust in which new stars and planets are forming. It is located about 1,500 light-years from Earth, which means the light recorded in the photograph took about 1,500 years to reach us. Thus, we see it as it was about 1,500 years ago. Photograph (b) sho ...
The white dwarf population within 40 pc of the Sun
... the total number of synthetic stars of the restricted samples described below and the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population we first generated a set of random posit ...
... the total number of synthetic stars of the restricted samples described below and the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population we first generated a set of random posit ...
A radiogenic heating evolution model for cosmochemically Earth
... et al., 1991). Because of the neutron densities required for the r-process to occur, it was originally suggested that this happens in the neutron-dense areas around neutron stars produced in supernovae (Burbidge et al., 1957). Other sites have been proposed such as binary neutron star or black hole ...
... et al., 1991). Because of the neutron densities required for the r-process to occur, it was originally suggested that this happens in the neutron-dense areas around neutron stars produced in supernovae (Burbidge et al., 1957). Other sites have been proposed such as binary neutron star or black hole ...
G030338-00 - DCC
... 90% confidence upper limit: inspiral rate < 170/year per Milky-way equivalent galaxy, in the (m1, m2) range of 1 to 3 solar masses. LIGO-G030338-00-R ...
... 90% confidence upper limit: inspiral rate < 170/year per Milky-way equivalent galaxy, in the (m1, m2) range of 1 to 3 solar masses. LIGO-G030338-00-R ...
Distances in Cosmology One of the most basic measurements that
... direction appears to change, by an amount that is inversely proportional to its distance from the viewing points. This is one of the ways we obtain depth perception; looking out with first one eye, then the other, shows that close things appear to move more than distant things. If you know the dista ...
... direction appears to change, by an amount that is inversely proportional to its distance from the viewing points. This is one of the ways we obtain depth perception; looking out with first one eye, then the other, shows that close things appear to move more than distant things. If you know the dista ...
POSTERS SESSION I: Atmospheres of Massive Stars
... Massive stars have strong stellar winds that exhibit variability on timescales ranging from hours to years. Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can indu ...
... Massive stars have strong stellar winds that exhibit variability on timescales ranging from hours to years. Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can indu ...
Section 7 - LISA Science Team
... Variations of the field propagate at the speed of light through gravitational waves (GW). • GW are related to the quadrupolar mass distribution of the source (no dipole-radiation: ...
... Variations of the field propagate at the speed of light through gravitational waves (GW). • GW are related to the quadrupolar mass distribution of the source (no dipole-radiation: ...
Using time to measure distance - AS-A2
... In the winter of the years 2000 to 2001 Jupiter and Saturn appeared very close together in the night sky. They were both in the south at midnight, which means that the Earth was directly between them and the Sun. This is called an ‘opposition’. It also means that the two planets were both at the sam ...
... In the winter of the years 2000 to 2001 Jupiter and Saturn appeared very close together in the night sky. They were both in the south at midnight, which means that the Earth was directly between them and the Sun. This is called an ‘opposition’. It also means that the two planets were both at the sam ...
The white dwarf population within 40 pc of the Sun
... the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population, we first generated a set of random positions of synthetic white dwarfs in a spherical region centered on the Sun, adoptin ...
... the observed sample are always similar. In this way we guarantee that the comparison of both sets of data are statistically sound. To produce a consistent white dwarf population, we first generated a set of random positions of synthetic white dwarfs in a spherical region centered on the Sun, adoptin ...
Astrophysical parameters of ten poorly studied open star clusters
... images. Star counts and photometric parameters (radius, membership, distance, color excess, age, luminosity function, mass function, total mass, and dynamical relaxation time) have been determined for these ten clusters for the first time. In order to calibrate our procedures, the main parameters (d ...
... images. Star counts and photometric parameters (radius, membership, distance, color excess, age, luminosity function, mass function, total mass, and dynamical relaxation time) have been determined for these ten clusters for the first time. In order to calibrate our procedures, the main parameters (d ...
Origin and evolution of magnetars
... The recent evidence for magnetic fluxes similar to those of the magnetars in a high fraction (∼25 per cent) of massive O-type stars lends support to such a hypothesis. Another possibility is that the spin of the neutron star is a strong function of the progenitor mass, and it is only for stars that ...
... The recent evidence for magnetic fluxes similar to those of the magnetars in a high fraction (∼25 per cent) of massive O-type stars lends support to such a hypothesis. Another possibility is that the spin of the neutron star is a strong function of the progenitor mass, and it is only for stars that ...
The white dwarf population within 40 pc of the Sun
... of both sets of data are statistically sound. To produce a consistent white dwarf population, we first generated a set of random positions of synthetic white dwarfs in a spherical region centered on the Sun, adopting a radius of 50 pc. We used a double exponential distribution for the local density ...
... of both sets of data are statistically sound. To produce a consistent white dwarf population, we first generated a set of random positions of synthetic white dwarfs in a spherical region centered on the Sun, adopting a radius of 50 pc. We used a double exponential distribution for the local density ...