Discovery of Eclipsing Binary with the Longest Known Period
... much more luminous F0I star. The eclipses in V383 Sco have different depth in various photometric bands, with the color index (V-I) changing by more than 1.5m between the maximum and minimum light. The principal difference between J0953+3353 and such systems is that the obscuring body of J0953+3353 ...
... much more luminous F0I star. The eclipses in V383 Sco have different depth in various photometric bands, with the color index (V-I) changing by more than 1.5m between the maximum and minimum light. The principal difference between J0953+3353 and such systems is that the obscuring body of J0953+3353 ...
Stellar populations in the nuclear regions of nearby radio galaxies
... 1990). The values found in Seyfert 1 nuclei are also consistent with this idea if the dilution produced by a nuclear non-stellar source is taken into account (Terlevich, Dı́az & Terlevich 1990; JiménezBenito et al. 2000). The high mass-to-light ratios L(1.6 mm)/M inferred in Seyfert 2 nuclei also i ...
... 1990). The values found in Seyfert 1 nuclei are also consistent with this idea if the dilution produced by a nuclear non-stellar source is taken into account (Terlevich, Dı́az & Terlevich 1990; JiménezBenito et al. 2000). The high mass-to-light ratios L(1.6 mm)/M inferred in Seyfert 2 nuclei also i ...
hr diagrams of star clusters
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
THE PERIOD OF ROTATION OF THE SUN
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
Test 4 Review Clicker Questions
... a) 21-cm maps of the spiral arms b) the rotation curve of the outer edges of the Galaxy c) orbits of open clusters in the disk d) infrared observations of new starforming regions e) X-ray images of other galaxies ...
... a) 21-cm maps of the spiral arms b) the rotation curve of the outer edges of the Galaxy c) orbits of open clusters in the disk d) infrared observations of new starforming regions e) X-ray images of other galaxies ...
HR DIAGRAMS OF STAR CLUSTERS
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
... Vireo has stored a wide range of isochrones that you can use to match against your cluster HR diagram. Once you have matched the zero-age main-sequence, you can then call up the isochrone-fitting tool. On the menu bar of the ColorMagnitude diagram window, call up Tools > Isochrones, and you will see ...
Oxford Meeting
... High Redshift Lyman- emission lines surveys: Astrophysical principles for Success Partridge and Peebles, 1967, Are Young Galaxies visible? [Basic idea has been around a long time] ...
... High Redshift Lyman- emission lines surveys: Astrophysical principles for Success Partridge and Peebles, 1967, Are Young Galaxies visible? [Basic idea has been around a long time] ...
ppt
... The Pleiades • An open cluster is a group of up to a few thousand stars that were formed from the same giant molecular cloud, and are still gravitationally bound to each other • Open clusters are found only in spiral and irregular galaxies, in which active star formation is occurring. • The Pleiad ...
... The Pleiades • An open cluster is a group of up to a few thousand stars that were formed from the same giant molecular cloud, and are still gravitationally bound to each other • Open clusters are found only in spiral and irregular galaxies, in which active star formation is occurring. • The Pleiad ...
New Suns in the Cosmos?
... upsurge along the past 15 years, with the discovery of many extra-solar planetary systems, demonstrating that the Sun is not unique as a planet host star. In this context, the main question now is the extent to which the properties of the Sun and its planetary system can be considered as representat ...
... upsurge along the past 15 years, with the discovery of many extra-solar planetary systems, demonstrating that the Sun is not unique as a planet host star. In this context, the main question now is the extent to which the properties of the Sun and its planetary system can be considered as representat ...
Evidence for the Tidal Destruction of Hot Jupiters by Subgiant Stars
... Figure 2. Galactic U V W kinematics of subgiant stars that host exoplanets discovered with the radial-velocity technique. In each panel, we plot the U V W space motions of the subgiant sample as blue points and the density of points in a control sample selected from the Hipparcos catalog as the back ...
... Figure 2. Galactic U V W kinematics of subgiant stars that host exoplanets discovered with the radial-velocity technique. In each panel, we plot the U V W space motions of the subgiant sample as blue points and the density of points in a control sample selected from the Hipparcos catalog as the back ...
Active Galactic Nuclei at kiloparsec scales and their cosmological
... The SKA will permit studying the neutral hydrogen content of galaxies to cosmological significant distances (z ∼2). A key tool will be the observation of this line in absorption in front of radio continuum sources. The chances of detecting the HI line at 21 cm in absorption is virtually redshift-ind ...
... The SKA will permit studying the neutral hydrogen content of galaxies to cosmological significant distances (z ∼2). A key tool will be the observation of this line in absorption in front of radio continuum sources. The chances of detecting the HI line at 21 cm in absorption is virtually redshift-ind ...
A CCD Search for Variable Stars of Spectral Type B in the Northern
... in B, 25 in U, and 24 in V, Hill (1967) found the star to be variable, derived a period of 0.39912 d (frequency 2.5055 d 1 ) and the amplitudes (half ranges) of 9 mmag and 8 mmag in B and U, respectively (no V amplitude was given). On the strength of these results, Hill (1967) classified the star as ...
... in B, 25 in U, and 24 in V, Hill (1967) found the star to be variable, derived a period of 0.39912 d (frequency 2.5055 d 1 ) and the amplitudes (half ranges) of 9 mmag and 8 mmag in B and U, respectively (no V amplitude was given). On the strength of these results, Hill (1967) classified the star as ...
Evolution of the Highest Redshift Quasars
... • First detection of complete G-P trough: SDSS J1030 (z=6.28, Becker et al. 2001) • G-P optical depth evolution of ionizing background and neutral fraction of the IGM ...
... • First detection of complete G-P trough: SDSS J1030 (z=6.28, Becker et al. 2001) • G-P optical depth evolution of ionizing background and neutral fraction of the IGM ...
3. Cosmology and the Origin and Evolution of Galaxies
... (SEDs) of mm galaxies at rest-frame mid-IR to radio wavelengths can provide photometric-redshifts with sufficient accuracy7. There has also been some success in the measurement of optical and IR spectroscopic redshifts for a fraction of the bright mm galaxies (S850µm > 5 mJy) with reliable radio coun ...
... (SEDs) of mm galaxies at rest-frame mid-IR to radio wavelengths can provide photometric-redshifts with sufficient accuracy7. There has also been some success in the measurement of optical and IR spectroscopic redshifts for a fraction of the bright mm galaxies (S850µm > 5 mJy) with reliable radio coun ...
PPT presentation
... Ford & Jenner (1975) followed up with deeper observations of NGC 221 (=M32), detecting 21 PNe in its field. 3 of the 14 PNe with observed radial velocities belonged to M31, the rest to NGC 221 (200 km/s difference between the two). ...
... Ford & Jenner (1975) followed up with deeper observations of NGC 221 (=M32), detecting 21 PNe in its field. 3 of the 14 PNe with observed radial velocities belonged to M31, the rest to NGC 221 (200 km/s difference between the two). ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... Al abundance present in the hydrogen shell is ejected unmodified in the supernova explosion or, in more massive stars during their Wolf-Rayet phase, by a stellar wind. The 26Al synthesized in the oxygen-neon shell may be significantly enhanced because of operation of the neutrino process (Woosley et ...
... Al abundance present in the hydrogen shell is ejected unmodified in the supernova explosion or, in more massive stars during their Wolf-Rayet phase, by a stellar wind. The 26Al synthesized in the oxygen-neon shell may be significantly enhanced because of operation of the neutrino process (Woosley et ...
Introduction: The History and Technique of Stellar Classification
... von Fraunhofer early in the 1800’s, but it was not until late in that century that astronomers were able to routinely examine the spectra of stars in large numbers. Astronomers Angelo Secchi and E.C. Pickering were among the first to note that stellar spectra could be divided into groups by their ge ...
... von Fraunhofer early in the 1800’s, but it was not until late in that century that astronomers were able to routinely examine the spectra of stars in large numbers. Astronomers Angelo Secchi and E.C. Pickering were among the first to note that stellar spectra could be divided into groups by their ge ...
Present
... Masses in red stars range from 8x1010 to 6x1011 Mo, if the mean stellar age is below 109 years, and significantly higher masses if the stars are older. They are probably young massive ellipticals in the final stages of star formation, where much of their stellar mass is already in place, yet very ...
... Masses in red stars range from 8x1010 to 6x1011 Mo, if the mean stellar age is below 109 years, and significantly higher masses if the stars are older. They are probably young massive ellipticals in the final stages of star formation, where much of their stellar mass is already in place, yet very ...
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.