Soft X-Ray Polarimetry
... and fraction that depend on how ordered the magnetic field is and whether relativistic shocks drive the emission of X-rays (§2.2). • “When and how did supermassive black holes grow?” New studies indicate that SMBH mass and spin may be determined using polarization measurements across the 0.1-10 keV ...
... and fraction that depend on how ordered the magnetic field is and whether relativistic shocks drive the emission of X-rays (§2.2). • “When and how did supermassive black holes grow?” New studies indicate that SMBH mass and spin may be determined using polarization measurements across the 0.1-10 keV ...
Measuring distances to the edge of the local group
... The formation of the solar system from the solar nebula has been notoriously difficult to model. The solar system is unique compared to other planetary system that we have observed, most of which have massive Jupiter-sized objects orbiting very closely to the host star. The prominent formation model ...
... The formation of the solar system from the solar nebula has been notoriously difficult to model. The solar system is unique compared to other planetary system that we have observed, most of which have massive Jupiter-sized objects orbiting very closely to the host star. The prominent formation model ...
Universe of Motion - Reciprocal System of theory
... This volume is a continuation of a series which undertakes to determine the characteristics that the physical universe must necessarily have if it is composed entirely of discrete units of motion, and to show that the universe thus defined is identical, item by item, with the observed physical unive ...
... This volume is a continuation of a series which undertakes to determine the characteristics that the physical universe must necessarily have if it is composed entirely of discrete units of motion, and to show that the universe thus defined is identical, item by item, with the observed physical unive ...
Article (Published version) - Archive ouverte UNIGE
... Measurements were obtained with the cross-dispersed echelle ELODIE spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence observatory (OHP, France) between late 1993 and mid 2006 (Baranne et al. 1996). The stars were subsequently monitored by the SOPHIE spectrograph that ...
... Measurements were obtained with the cross-dispersed echelle ELODIE spectrograph mounted on the 1.93-m telescope at the Observatoire de Haute-Provence observatory (OHP, France) between late 1993 and mid 2006 (Baranne et al. 1996). The stars were subsequently monitored by the SOPHIE spectrograph that ...
A spectroscopic investigation of the O-type star - ORBi
... intense survey of the stars but also a good time sampling to constrain the short- as well as the long-period systems. This monitoring has to be as homogeneous as possible because combining data from the literature may provide erroneous results. Indeed, the literature (especially the older papers) of ...
... intense survey of the stars but also a good time sampling to constrain the short- as well as the long-period systems. This monitoring has to be as homogeneous as possible because combining data from the literature may provide erroneous results. Indeed, the literature (especially the older papers) of ...
The Multitude of Molecular Hydrogen Knots in the Helix Nebula 1
... picture of the cometary knots reveals that they are neutral gas condensations that appear as comet like structures with rims bright in Hα and tails that appear as shadows in [OIII] and that point away from the central star. The rim of low-excitation ionize gas has a steep temperature gradient indica ...
... picture of the cometary knots reveals that they are neutral gas condensations that appear as comet like structures with rims bright in Hα and tails that appear as shadows in [OIII] and that point away from the central star. The rim of low-excitation ionize gas has a steep temperature gradient indica ...
Heating and Cooling of Neutron Star Crusts
... A theoretical crust model was developed in this work to follow the evolution of the quiescent luminosity of a transiently accreting neutron star, and its results were compared with observations of two transient neutron stars: KS 1731-260 and MXB 1659-298. The comparison shows that the calculations f ...
... A theoretical crust model was developed in this work to follow the evolution of the quiescent luminosity of a transiently accreting neutron star, and its results were compared with observations of two transient neutron stars: KS 1731-260 and MXB 1659-298. The comparison shows that the calculations f ...
on the absolute age of the metal-rich globular m71
... We investigated the absolute age of the Galactic globular cluster M71 (NGC 6838) using optical ground-based images (u¢ , g¢ , r ¢ , i¢ , z ¢) collected with the MegaCam camera at the Canada–France–Hawaii Telescope (CFHT). We performed a robust selection of field and cluster stars by applying a new me ...
... We investigated the absolute age of the Galactic globular cluster M71 (NGC 6838) using optical ground-based images (u¢ , g¢ , r ¢ , i¢ , z ¢) collected with the MegaCam camera at the Canada–France–Hawaii Telescope (CFHT). We performed a robust selection of field and cluster stars by applying a new me ...
Hubble Space Telescope Imaging of Post
... We investigate a sample of objects in this paper at somewhat lower redshifts and luminosities than the prototype thus it is necessary to consider the premise of Hasinger (2008). It seems that while major merger-driven evolution dominates in the early universe, producing the bulk of the brightest qua ...
... We investigate a sample of objects in this paper at somewhat lower redshifts and luminosities than the prototype thus it is necessary to consider the premise of Hasinger (2008). It seems that while major merger-driven evolution dominates in the early universe, producing the bulk of the brightest qua ...
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. ...
EL CVn-type binaries - Discovery of 17 helium white dwarf
... is eclipsed by a 0.945M⊙ star with an effective temperature Teff = 9370 K. The eclipsing binary star AW UMa may also contain a pre-He-WD, although the interpretation of this system is complicated by an equatorial belt of material that makes the lightcurve of this binary look like that of a W UMa-typ ...
... is eclipsed by a 0.945M⊙ star with an effective temperature Teff = 9370 K. The eclipsing binary star AW UMa may also contain a pre-He-WD, although the interpretation of this system is complicated by an equatorial belt of material that makes the lightcurve of this binary look like that of a W UMa-typ ...
6.7 GHz Methanol Masers and the GBT
... Methanol masers at 6.7 GHz • Since these methanol masers are often not associated with infrared emission, they are best discovered using blind surveys. • To date, there have been only around four blind surveys carried out to detect 6.7 GHz methanol masers. • Most of the other surveys are targeted t ...
... Methanol masers at 6.7 GHz • Since these methanol masers are often not associated with infrared emission, they are best discovered using blind surveys. • To date, there have been only around four blind surveys carried out to detect 6.7 GHz methanol masers. • Most of the other surveys are targeted t ...
PART TWO: No Singularity inside Black Holes (BH)
... equilibrium of OIC in our universal BH, they may be used to research the equilibrium and the physical states in star-formed BHs too. No OIC in universe can directly contract to become a BH. In the processes of its contraction, there are many strong resistances. OIC contains about ¾ hydrogen (H2). Wh ...
... equilibrium of OIC in our universal BH, they may be used to research the equilibrium and the physical states in star-formed BHs too. No OIC in universe can directly contract to become a BH. In the processes of its contraction, there are many strong resistances. OIC contains about ¾ hydrogen (H2). Wh ...
Evolution of high-redshift quasars
... 6 SDSS quasars ranging from several times 108 M to several times 109 M . Assuming continuous Eddington accretion from a seed black hole of 100 M , the formation redshift for seed black holes must be at z > 10. Even with continuous accretion, black holes in the most luminous quasars barely had eno ...
... 6 SDSS quasars ranging from several times 108 M to several times 109 M . Assuming continuous Eddington accretion from a seed black hole of 100 M , the formation redshift for seed black holes must be at z > 10. Even with continuous accretion, black holes in the most luminous quasars barely had eno ...
Periodic Universal Gravitation Resulting in the Phenomenon of Dark
... 1) dr/dt conducted from the periodic universal gravitation on two objects m1 and m2 is independent of m1 and m2, indicating the dr/dt is the speed of cosmic expansion. So equation (3) is referred to as the cosmic expansion equation. 2) The cosmic expansion acceleration d2r/dt2 is negative. A vacuum ...
... 1) dr/dt conducted from the periodic universal gravitation on two objects m1 and m2 is independent of m1 and m2, indicating the dr/dt is the speed of cosmic expansion. So equation (3) is referred to as the cosmic expansion equation. 2) The cosmic expansion acceleration d2r/dt2 is negative. A vacuum ...
Fundamental properties of core-collapse Supernova and GRB
... RSG phase. The models predict that core-collapse SN occur after the WR phase, and are of the type Ibc (Georgy et al. 2012, 2009). However, this scenario has yet to be observationally confirmed, specially because WR stars have not been directly detected as SN Ibc progenitors yet (Smartt 2009; Eldridg ...
... RSG phase. The models predict that core-collapse SN occur after the WR phase, and are of the type Ibc (Georgy et al. 2012, 2009). However, this scenario has yet to be observationally confirmed, specially because WR stars have not been directly detected as SN Ibc progenitors yet (Smartt 2009; Eldridg ...
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.