Sample
... Confirming that a black hole exists at the center of the Milky Way galaxy has proven to be quite challenging. Because black holes are dark objects, they cannot be observed directly. Furthermore, because of extinction by interstellar clouds of gas and dust, the galaxy’s core is hidden from our view a ...
... Confirming that a black hole exists at the center of the Milky Way galaxy has proven to be quite challenging. Because black holes are dark objects, they cannot be observed directly. Furthermore, because of extinction by interstellar clouds of gas and dust, the galaxy’s core is hidden from our view a ...
Final Paper Template for the 5th Southeast Asian Forum
... dynamical evolution under influence of Galactic tidal field. If the internal bonding of the cluster is stronger than the external field, it has greater probability to survive. The other way, smaller cluster with few member will dissolve and come to an end which is known as open cluster remnant (OCR) ...
... dynamical evolution under influence of Galactic tidal field. If the internal bonding of the cluster is stronger than the external field, it has greater probability to survive. The other way, smaller cluster with few member will dissolve and come to an end which is known as open cluster remnant (OCR) ...
A Deeper Look at Faint H $\ alpha $ Emission in Nearby Dwarf
... Observations were conducted between 2010 March 11-15. New moon occurred on the night of March 15. Observing conditions were photometric through the run. The seeing was generally quite good (0.′′ 6-0.′′ 7), though there were increases up to ∼1.′′ 2 on the later halves of the first two nights. The MMT ...
... Observations were conducted between 2010 March 11-15. New moon occurred on the night of March 15. Observing conditions were photometric through the run. The seeing was generally quite good (0.′′ 6-0.′′ 7), though there were increases up to ∼1.′′ 2 on the later halves of the first two nights. The MMT ...
What, and Why, is the International Astronomical Union?
... cohort of officers, immediately self-destructed. Solar Radiation (Comm. 10) chose almost immediately to merge with Solar Physics (Comm. 12), leaving the set shown in the table at the time of the 1925 General Assembly, where two more, dealing with the structure of the Milky Way and diffuse matter in ...
... cohort of officers, immediately self-destructed. Solar Radiation (Comm. 10) chose almost immediately to merge with Solar Physics (Comm. 12), leaving the set shown in the table at the time of the 1925 General Assembly, where two more, dealing with the structure of the Milky Way and diffuse matter in ...
Mass-radius Relations for Helium White Dwarfs
... relationship between the mass and radius of a white dwarf is important in interpreting some of the observational results. M-R relation was first defined by Chandrasekhar [4]. Later Hamada and Salpeter [5] obtained numerical models for different core compositions by considering a fully degenerate con ...
... relationship between the mass and radius of a white dwarf is important in interpreting some of the observational results. M-R relation was first defined by Chandrasekhar [4]. Later Hamada and Salpeter [5] obtained numerical models for different core compositions by considering a fully degenerate con ...
STELLAR AGE VERSUS MASS OF EARLY
... performed visually by allowing age steps of 0.05 dex. The age range was then kept fixed for the other colors (middle and bottom panel). We see from the top panel of Fig. 2 that the SSP of HPL07 exceeds the observed color range at intermediate ages. This is no surprise, though: since the reddest colo ...
... performed visually by allowing age steps of 0.05 dex. The age range was then kept fixed for the other colors (middle and bottom panel). We see from the top panel of Fig. 2 that the SSP of HPL07 exceeds the observed color range at intermediate ages. This is no surprise, though: since the reddest colo ...
First astronomical unit scale image of the GW Orionis triple system
... 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry. Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resol ...
... 2003, 2004, and 2005. By measuring squared visibilities and closure phases with a good UV coverage we carry out the first image reconstruction of GW Ori from infrared long-baseline interferometry. Results. We obtained the first infrared image of a T Tauri multiple system with astronomical unit resol ...
The white dwarf cooling sequence of 47 Tucanae
... which white dwarfs are cooling. They assumed a constant white dwarf formation rate. Thus, the position in the sorted list is proportional to the time spent on the cooling sequence. Their sorted, completeness-corrected distribution of effective temperatures is shown Fig. 2 as a grey shaded band, whic ...
... which white dwarfs are cooling. They assumed a constant white dwarf formation rate. Thus, the position in the sorted list is proportional to the time spent on the cooling sequence. Their sorted, completeness-corrected distribution of effective temperatures is shown Fig. 2 as a grey shaded band, whic ...
AGN surveys to study galaxy evolution along cosmic times
... star formation and black hole accretion. The long wavelengths of these lines, ranging from the far-IR for the photodissociation and HII region lines, through the mid-IR for the AGN lines, to the near-IR for the coronal lines, ensure that we can observe these different tracers by minimising the effect ...
... star formation and black hole accretion. The long wavelengths of these lines, ranging from the far-IR for the photodissociation and HII region lines, through the mid-IR for the AGN lines, to the near-IR for the coronal lines, ensure that we can observe these different tracers by minimising the effect ...
HWWS 2010 - Monash University
... • Latter two are both likely classes of magnetars, (possibly young) systems with extremely high magnetic fields 1014– 1015 G • Compact central objects (CCOs) about which very little is known, associated with supernova remnants Galloway, “Accreting Neutron Stars – tiny Galactic Powerhouses” ...
... • Latter two are both likely classes of magnetars, (possibly young) systems with extremely high magnetic fields 1014– 1015 G • Compact central objects (CCOs) about which very little is known, associated with supernova remnants Galloway, “Accreting Neutron Stars – tiny Galactic Powerhouses” ...
THE ORION NEBULA AND ITS ASSOCIATED POPULATION C. R. O
... There have been major reviews of our knowledge of the object, two outstanding examples being the compilation of material by Goudis (1982) into a source book and the proceedings of the symposium marking the centennial of the first photographic images of M 42 (Glassgold et al. 1982). Earlier volumes o ...
... There have been major reviews of our knowledge of the object, two outstanding examples being the compilation of material by Goudis (1982) into a source book and the proceedings of the symposium marking the centennial of the first photographic images of M 42 (Glassgold et al. 1982). Earlier volumes o ...
Dai, S - PulsarAstronomy.net
... 2012, American Astronomical Society Meeting Abstracts, 220, #307.03 ...
... 2012, American Astronomical Society Meeting Abstracts, 220, #307.03 ...
Phases of Stellar Evolution
... For the pp cycle at 4(106) < T < 2.4(107) K 6 n 3.5 in ε= ε0ρTn This means that the temperature gradient is much smaller. There is less centralization in the energy generation and little tendency for convection in the core. pp cores are radiative ...
... For the pp cycle at 4(106) < T < 2.4(107) K 6 n 3.5 in ε= ε0ρTn This means that the temperature gradient is much smaller. There is less centralization in the energy generation and little tendency for convection in the core. pp cores are radiative ...
HST Key Project to Measure the Hubble Constant from
... – Supernova from massive stars, fainter and show wider variation in luminosity than IaSN – Baade-Wesselink technique: follow spectral fits of color T, flux and radial vel of envelope over time to det dist. – Applied independent of local calibration of extragalactic distance scale but verified with g ...
... – Supernova from massive stars, fainter and show wider variation in luminosity than IaSN – Baade-Wesselink technique: follow spectral fits of color T, flux and radial vel of envelope over time to det dist. – Applied independent of local calibration of extragalactic distance scale but verified with g ...
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.