arXiv 2011 Feroci
... are also observed during type I X-ray bursts, which are mostly the result of thermally unstable helium ignition in the accreted envelope of a neutron star. This generates a thermonuclear explosion that is observed as an X-ray burst with a rapid rise (∼1 s) followed by a slower decay (∼10–100 s). X-r ...
... are also observed during type I X-ray bursts, which are mostly the result of thermally unstable helium ignition in the accreted envelope of a neutron star. This generates a thermonuclear explosion that is observed as an X-ray burst with a rapid rise (∼1 s) followed by a slower decay (∼10–100 s). X-r ...
Practical cosmology with the Local Volume galaxies
... While having accurate velocities and distances for ~250 LV galaxies, one can study distribution of peculiar velocities within the Volume. A peculiar velocity map for the LV galaxies in the LG reference frame shows the local Hubble flow to be generally calm with peculiar velocity variations within ± ...
... While having accurate velocities and distances for ~250 LV galaxies, one can study distribution of peculiar velocities within the Volume. A peculiar velocity map for the LV galaxies in the LG reference frame shows the local Hubble flow to be generally calm with peculiar velocity variations within ± ...
Research Papers-Cosmology/Download/6307
... directly from the observations, is a spiral galaxy in which stars visualized the boundary of the core of the vortex of the dark gas. The observations show that the stars in the nucleus of the spiral galaxies rotate around a common center under the law of the rotation of a rigid body and only the sta ...
... directly from the observations, is a spiral galaxy in which stars visualized the boundary of the core of the vortex of the dark gas. The observations show that the stars in the nucleus of the spiral galaxies rotate around a common center under the law of the rotation of a rigid body and only the sta ...
Two New Triple Star Systems with Detectable Inner Orbital Motions
... The internal precision errors were less than the external accuracy errors by a factor of eight. It might be noted that, if instead of considering the variance within single data cubes, precision had been estimated by comparing the repeatability of observations of the same binaries across several nig ...
... The internal precision errors were less than the external accuracy errors by a factor of eight. It might be noted that, if instead of considering the variance within single data cubes, precision had been estimated by comparing the repeatability of observations of the same binaries across several nig ...
Starfarer
... How high a star may rise and still be of use for steering, and therefore how many stars in succession are needed is dependent on the direction of the course and the latitude. While from the equator the apparent motion of starts is vertical, at the south latitudes of the pacific islands, it is seen t ...
... How high a star may rise and still be of use for steering, and therefore how many stars in succession are needed is dependent on the direction of the course and the latitude. While from the equator the apparent motion of starts is vertical, at the south latitudes of the pacific islands, it is seen t ...
First axion bounds from a pulsating helium
... particles to dark matter is dependent on their mass (or coupling constant). However, the models do not provide information about the value of the axion mass, and therefore it has to be inferred from observations. In particular, stars can be employed to place constraints on the mass of the axion [8, ...
... particles to dark matter is dependent on their mass (or coupling constant). However, the models do not provide information about the value of the axion mass, and therefore it has to be inferred from observations. In particular, stars can be employed to place constraints on the mass of the axion [8, ...
The peculiar dipping events in the disc-bearing young
... 2012). Our target is a single star (Kraus & Hillenbrand 2007) of spectral type M1 and has a logarithmic bolometric stellar luminosity logL /L = 0.15 (Preibisch et al. 2002). The inferred radius of this star is R = 0.97 R , while the stellar mass is M ∼ 0.5 M , depending on the evolutionary mod ...
... 2012). Our target is a single star (Kraus & Hillenbrand 2007) of spectral type M1 and has a logarithmic bolometric stellar luminosity logL /L = 0.15 (Preibisch et al. 2002). The inferred radius of this star is R = 0.97 R , while the stellar mass is M ∼ 0.5 M , depending on the evolutionary mod ...
CH12.AST1001.F16.EDS
... A. It would be only 1/3 as bright. B. It would be only 1/6 as bright. C. It would be only 1/9 as bright. D. It would be three times as bright. ...
... A. It would be only 1/3 as bright. B. It would be only 1/6 as bright. C. It would be only 1/9 as bright. D. It would be three times as bright. ...
The stellar populations in the low-luminosity, early
... which are much fainter than our original sample of LLEs, and have stellar masses of only a few × 107 M or less (
... which are much fainter than our original sample of LLEs, and have stellar masses of only a few × 107 M or less (
The effect of the environment on the HI scaling relations
... already known, but a detailed quantification of their properties, crucial for a comparison with models, was still missing. Luckily, the situation is rapidly changing for 21 cm studies. The advent of large Hi surveys, such as the Arecibo Legacy Fast ALFA Survey (Giovanelli et al. 2005), which eventua ...
... already known, but a detailed quantification of their properties, crucial for a comparison with models, was still missing. Luckily, the situation is rapidly changing for 21 cm studies. The advent of large Hi surveys, such as the Arecibo Legacy Fast ALFA Survey (Giovanelli et al. 2005), which eventua ...
Separating gas-giant and ice-giant planets by halting pebble accretion
... & Valenti 2005; Buchhave et al. 2012). However, from a theoretical perspective it is poorly understood how the core accretion scenario could have taken place, if the cores grew by accretion of km-sized planetesimals and their fragments. Protoplanetary disc life-times range from ∼3 Myr (Haisch et al. ...
... & Valenti 2005; Buchhave et al. 2012). However, from a theoretical perspective it is poorly understood how the core accretion scenario could have taken place, if the cores grew by accretion of km-sized planetesimals and their fragments. Protoplanetary disc life-times range from ∼3 Myr (Haisch et al. ...
the red supergiant content of m31
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
... stars lose most of their hydrogen-rich envelopes and exploded instead as type II-L or even type Ib supernovae. The validity of this resolution rests on the assumption that the RSG mass-loss rates have been seriously underestimated. Meynet et al. (2015) and Georgy et al. (2015) proposed a novel way o ...
Five New Extrasolar Planets
... Butler et al. 1996). The method involves placing Iodine molecules at pressure of 0.01 atm in an absorption cell at a temperature of 50 C in front of the focal plane of the Keck 1 telescope, centered on the optical axis, to superimpose iodine lines on the stellar spectrum. The pyrex Iodine cell is se ...
... Butler et al. 1996). The method involves placing Iodine molecules at pressure of 0.01 atm in an absorption cell at a temperature of 50 C in front of the focal plane of the Keck 1 telescope, centered on the optical axis, to superimpose iodine lines on the stellar spectrum. The pyrex Iodine cell is se ...
Chapter 12: Surveying the Stars 12.1 Properties of Stars How do we
... © 2015 Pearson Education, Inc. ...
... © 2015 Pearson Education, Inc. ...
An evolutionary channel towards the accreting millisecond pulsar
... angular momentum of the pulsar (Tauris & Savonije 1999), while the donor-star winds were assumed to be ejected from the inner Lagrangian point by the radiation pressure of the pulsar (Burderi & Possenti 2001), and carry away the specific orbital angular momentum at this point (Burderi et al. 2002; J ...
... angular momentum of the pulsar (Tauris & Savonije 1999), while the donor-star winds were assumed to be ejected from the inner Lagrangian point by the radiation pressure of the pulsar (Burderi & Possenti 2001), and carry away the specific orbital angular momentum at this point (Burderi et al. 2002; J ...
FIRST DETECTION OF KRYPTON AND XENON IN A WHITE DWARF
... phase of the previous evolution. They also pointed out that this phenomenon is obviously restricted to DO WDs. This can be understood when considering that their immediate progenitors, the PG1159 stars, also show signs of n-capture nucleosynthesis in the light-metal abundance patterns (Werner & Herw ...
... phase of the previous evolution. They also pointed out that this phenomenon is obviously restricted to DO WDs. This can be understood when considering that their immediate progenitors, the PG1159 stars, also show signs of n-capture nucleosynthesis in the light-metal abundance patterns (Werner & Herw ...
Star formation
Star formation is the process by which dense regions within molecular clouds in interstellar space, sometimes referred to as ""stellar nurseries"" or ""star-forming regions"", collapse to form stars. As a branch of astronomy, star formation includes the study of the interstellar medium (ISM) and giant molecular clouds (GMC) as precursors to the star formation process, and the study of protostars and young stellar objects as its immediate products. It is closely related to planet formation, another branch of astronomy. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of binary stars and the initial mass function.In June 2015, astronomers reported evidence for Population III stars in the Cosmos Redshift 7 galaxy at z = 6.60. Such stars are likely to have existed in the very early universe (i.e., at high redshift), and may have started the production of chemical elements heavier than hydrogen that are needed for the later formation of planets and life as we know it.