4. in-flight calibration plan
... analysis of CIPS angular distributions at a single wavelength will yield column mass and surface area. ...
... analysis of CIPS angular distributions at a single wavelength will yield column mass and surface area. ...
The new Basel high-latitude field star survey of the Galaxy
... Abstract. We discuss star count and three-color data for the two inner-Galaxy fields SA 107 and NGC 6171 observed in the new Basel RGU high-latitude field star survey. Our analysis is based on the structural models of the Galactic population components that were derived from the previous studies of ...
... Abstract. We discuss star count and three-color data for the two inner-Galaxy fields SA 107 and NGC 6171 observed in the new Basel RGU high-latitude field star survey. Our analysis is based on the structural models of the Galactic population components that were derived from the previous studies of ...
Applications of Photospheric Spot Temperature Models ... Stellar Angular Momentum Evolution
... 1.1 The Magnetic Disk-Locking Model and the Angular Momentum Conundrum 1.2 Observed Rotation Period Distributions of CTTS and WTTS ...
... 1.1 The Magnetic Disk-Locking Model and the Angular Momentum Conundrum 1.2 Observed Rotation Period Distributions of CTTS and WTTS ...
Luminosities and mass-loss rates of SMC and LMC AGB stars and
... in the LMC and SMC. In this paper we consider the currently publically available data from the following programmes: 200 (P.I. J. Houck), 3277 (P.I. M. Egan), 3426 (P.I. J. Kastner), 3505 (P.I. P. Wood), and 3591 (P.I. F. Kemper). The data in these programs are described by Sloan et al. (2008, progr ...
... in the LMC and SMC. In this paper we consider the currently publically available data from the following programmes: 200 (P.I. J. Houck), 3277 (P.I. M. Egan), 3426 (P.I. J. Kastner), 3505 (P.I. P. Wood), and 3591 (P.I. F. Kemper). The data in these programs are described by Sloan et al. (2008, progr ...
Proficiency Step #5--
... We tend to think of constellations as a group of related stars that form a pattern, when in fact, most of the constellations consist of stars that are not related—that is, they are varying distances from Earth and their relative positions are simply a coincidence. It might be convenient to note her ...
... We tend to think of constellations as a group of related stars that form a pattern, when in fact, most of the constellations consist of stars that are not related—that is, they are varying distances from Earth and their relative positions are simply a coincidence. It might be convenient to note her ...
Trapezium Fracture
... nebula. Within M42 are thousands of protostars and young stars, less than one million years old. Will one of these stars in a far distant time provide the conditions that allow the evolution of life on one of its planets, long after our own Earth has ceased to exist? Will the product of this evoluti ...
... nebula. Within M42 are thousands of protostars and young stars, less than one million years old. Will one of these stars in a far distant time provide the conditions that allow the evolution of life on one of its planets, long after our own Earth has ceased to exist? Will the product of this evoluti ...
The Milky Way - The Independent School
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect answers to five essential questions: ...
... Our Milky Way Galaxy is only one of the many billions of galaxies visible in the sky. This chapter will expand your horizon to discuss the different kinds of galaxies and their complex histories. Here you can expect answers to five essential questions: ...
talk at lensing and dark matter conference Ohio state 2004
... • Main conclusion: Macho’s as main component of Dark Matter are ruled out • But found significant extra microlensing ...
... • Main conclusion: Macho’s as main component of Dark Matter are ruled out • But found significant extra microlensing ...
... of the minerals, but are instead interference colors caused by the optical properties of the minerals and the polarized light of the microscope.) Note the presence of numerous large crystals in each chondrule. Melting and crystallization experiments show that such mineral shapes and sizes can be pro ...
The Kuiper Belt Explored by Serendipitous Stellar Occultations
... The angular sizes of the stars depend on their spectral and luminosity class and on their distance (see section 2.5). Figure 1 shows that, for a large proportion of stars, there would be full extinction for KBOs under 1 km in radius if the occultation were purely geometrical in nature. In reality, d ...
... The angular sizes of the stars depend on their spectral and luminosity class and on their distance (see section 2.5). Figure 1 shows that, for a large proportion of stars, there would be full extinction for KBOs under 1 km in radius if the occultation were purely geometrical in nature. In reality, d ...
adc - VizieR
... (SRa-d), the catalog usually gives one of the most recent epochs of maximum light. Epochs for novae (types N) and supernovae (types SN) are given in Julian days followed by a year of outburst enclosed in parentheses (bytes 109-114). The data field structure is as ...
... (SRa-d), the catalog usually gives one of the most recent epochs of maximum light. Epochs for novae (types N) and supernovae (types SN) are given in Julian days followed by a year of outburst enclosed in parentheses (bytes 109-114). The data field structure is as ...
Evolution in circumstellar envelopes of Be stars: From disks to rings?
... wings were present again, which is a reliable indicator of a new outburst à la µ Cen (Rivinius et al. 1998a). At the same time the Fe ii and Si ii line emission reappeared with a large width. The narrower doublepeaked emission in O i 8446 had lost a bit in width and two-thirds in peak height. But i ...
... wings were present again, which is a reliable indicator of a new outburst à la µ Cen (Rivinius et al. 1998a). At the same time the Fe ii and Si ii line emission reappeared with a large width. The narrower doublepeaked emission in O i 8446 had lost a bit in width and two-thirds in peak height. But i ...
EVIDENCE FOR IMF VARIATIONS WITH GALACTIC ENVIRONMENT
... on the physical properties of the stellar birth cloud such as the gas density, metallicity, or turbulent velocity (e.g.,; Larson 2005; Bate 2009; Myers et al. 2011; Marks et al. 2012; Hopkins 2012), however, IMF observations are largely invariant within the Milky Way (Bochanski et al. 2010; Covey et ...
... on the physical properties of the stellar birth cloud such as the gas density, metallicity, or turbulent velocity (e.g.,; Larson 2005; Bate 2009; Myers et al. 2011; Marks et al. 2012; Hopkins 2012), however, IMF observations are largely invariant within the Milky Way (Bochanski et al. 2010; Covey et ...
Astronomy Astrophysics − Orbital phase-resolved spectroscopy of 4U 1538
... values in the rest of this work. The soft excess at low energies (0.1−1 keV) presents in 4U 1538−52, and other HMXBs has not been considered here because it lies outside the energy range of the MAXI/GSC spectrum. Nevertheless, the well known fundamental cyclotron resonant-scattering feature (CRSF) a ...
... values in the rest of this work. The soft excess at low energies (0.1−1 keV) presents in 4U 1538−52, and other HMXBs has not been considered here because it lies outside the energy range of the MAXI/GSC spectrum. Nevertheless, the well known fundamental cyclotron resonant-scattering feature (CRSF) a ...
Radiative Precession of an Isolated Neutron Star
... field gradients (e.g. between the poles and equator if the field is a dipole) support non-radial matter-density gradients in hydromagnetic equilibrium. (This is not related in any way to the electromagnetic inertia of the external radiation fields discussed in Section 2.2.) The geometry and magnitud ...
... field gradients (e.g. between the poles and equator if the field is a dipole) support non-radial matter-density gradients in hydromagnetic equilibrium. (This is not related in any way to the electromagnetic inertia of the external radiation fields discussed in Section 2.2.) The geometry and magnitud ...
Spectral Matching for Elemental Abundances of Evolved Stars of Globular Clusters
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
... used to estimate the oxygen abundance of the stars, leading to a determination of whether a particular star was oxygen-rich or oxygen-poor. From this a catalogue of abundances of iron, carbon and barium of 848 giant branch stars were determined, of which 557 also had well-defined nitrogen abundances ...
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.