Isotopic composition of Hg and Pt in 5 slowly rotating HgMn stars *
... tected in any of them. More than 50% of the HgMn stars are members of either spectroscopic binary systems (SBs), many of which are double-lined systems (SB2s), or of systems of higher multiplicity, in which they are found in unusually high proportion (Hubrig & Mathys 1995). Another important distinc ...
... tected in any of them. More than 50% of the HgMn stars are members of either spectroscopic binary systems (SBs), many of which are double-lined systems (SB2s), or of systems of higher multiplicity, in which they are found in unusually high proportion (Hubrig & Mathys 1995). Another important distinc ...
Astronomy 114 - Department of Astronomy
... Interstellar gas and dust are common in the disk of the Galaxy Interstellar medium (ISM) Diffuse gas (atomic H and molecular hydrogen H2 ) Dust (formed in the envelopes of stars) ...
... Interstellar gas and dust are common in the disk of the Galaxy Interstellar medium (ISM) Diffuse gas (atomic H and molecular hydrogen H2 ) Dust (formed in the envelopes of stars) ...
ppt
... thus the temperature. In transit searching you need to find the right kind of stars (cool main sequence stars). Often you have to rely on color photometry ...
... thus the temperature. In transit searching you need to find the right kind of stars (cool main sequence stars). Often you have to rely on color photometry ...
Period analysis of variable stars by robust smoothing
... two eclipses and (2) the difference of amplitude between the primary minimum and the secondary minimum. The light curve (the solid line in the top panel) by SuperSmoother has almost the same amplitudes between two minima and is rounded between eclipses, while the light curves fitted by other smoothi ...
... two eclipses and (2) the difference of amplitude between the primary minimum and the secondary minimum. The light curve (the solid line in the top panel) by SuperSmoother has almost the same amplitudes between two minima and is rounded between eclipses, while the light curves fitted by other smoothi ...
white dwarfs and the age of the universe
... the interstellar medium [9], winds and so on. There is now a broad opinion that the distinction among the character DA and non–DA is inherited (i.e., it is linked to the origin of the white dwarf itself) although a fraction of them can change their external aspect during the evolution [10]. Standard ...
... the interstellar medium [9], winds and so on. There is now a broad opinion that the distinction among the character DA and non–DA is inherited (i.e., it is linked to the origin of the white dwarf itself) although a fraction of them can change their external aspect during the evolution [10]. Standard ...
Lives of Stars - McDonald Observatory
... heats up all the surrounding gas. APOLLO: Eventually, the energy makes it to our photospheres where it escapes as light into interstellar space. PAGE: Wait, so this has happened to all three of you? ...
... heats up all the surrounding gas. APOLLO: Eventually, the energy makes it to our photospheres where it escapes as light into interstellar space. PAGE: Wait, so this has happened to all three of you? ...
to - NexStar Resource Site
... 4) Saturn An object in our very own neighborhood in the constellation.......pick one. :-). Although Galileo was the first to observe it with a telescope in 1610, Saturn has been known since prehistoric times. Up to 1977 Saturn was believed to be the only planet with a ring system. It was later disc ...
... 4) Saturn An object in our very own neighborhood in the constellation.......pick one. :-). Although Galileo was the first to observe it with a telescope in 1610, Saturn has been known since prehistoric times. Up to 1977 Saturn was believed to be the only planet with a ring system. It was later disc ...
preprint, pdf version - LESIA
... the brighter magnitudes, then stars fainter than say R = 15−16 will always be left out of the candidate search. This is far from ideal in the case of TNOs. In contrast to Pluto occultations, for TNOs we obtain good contrast in the light curves using very modest instruments for stars as faint as R = ...
... the brighter magnitudes, then stars fainter than say R = 15−16 will always be left out of the candidate search. This is far from ideal in the case of TNOs. In contrast to Pluto occultations, for TNOs we obtain good contrast in the light curves using very modest instruments for stars as faint as R = ...
KIC 10449976: discovery of an extreme helium
... objects using the Isaac Newton Telescope (INT) in La Palma. One of the targets, KIC 10449976 (α = 18h 47m 14.s 1, δ = +47◦ 41 46. 9: J2000, g = 14.49), was observed because it was clearly blue (g − E-mail: [email protected] ...
... objects using the Isaac Newton Telescope (INT) in La Palma. One of the targets, KIC 10449976 (α = 18h 47m 14.s 1, δ = +47◦ 41 46. 9: J2000, g = 14.49), was observed because it was clearly blue (g − E-mail: [email protected] ...
Finnish Centre for Astronomy with ESO
... The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of the University of Turku, and funded by the Ministry of Education and Culture, and by the participating universities (Aalto, Helsinki, Oulu and Turku). The highest decision-making body is the Board, chaired b ...
... The year 2014 marked the 5th year of operation for FINCA, administratively a Special Unit of the University of Turku, and funded by the Ministry of Education and Culture, and by the participating universities (Aalto, Helsinki, Oulu and Turku). The highest decision-making body is the Board, chaired b ...
Comparing stars - The Open University
... If you knew that a red giant was larger than a main sequence star of comparable temperature, what could you say about its luminosity? View answer - Question 3 The bright star Aldebaran A ( Tau) is a red giant. (It's actually a visual binary, but the red giant is dominant.) Above and to the left of t ...
... If you knew that a red giant was larger than a main sequence star of comparable temperature, what could you say about its luminosity? View answer - Question 3 The bright star Aldebaran A ( Tau) is a red giant. (It's actually a visual binary, but the red giant is dominant.) Above and to the left of t ...
Spectroscopy: Unlocking the Secrets of Star Light
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
Spectroscopy: Unlocking the Secrets of Star Light
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
... A 10,000 K star would have its peak wavelength in the ultraviolet part of the em spectrum whilst a 3,000 K star would emit most of its radiation in the infrared part. Not only does the shape of the curve determine the relative intensity of the different components of the continuous spectrum produced ...
Exploring the Universe
... – Distance affects the brightness of stars – What we see is called the apparent magnitude – Absolute magnitude is a measurement of the brightness as if the distance from the earth was 32.6 light years away. A uniform distance, so it’s the real brightness. – Besides the sun, the brightest star is Sir ...
... – Distance affects the brightness of stars – What we see is called the apparent magnitude – Absolute magnitude is a measurement of the brightness as if the distance from the earth was 32.6 light years away. A uniform distance, so it’s the real brightness. – Besides the sun, the brightest star is Sir ...
Riccioli Measures the Stars: Observations of the
... the stars dwarf the orbit of the Earth.* Riccioli also critiques Landsbergius who cites naked eye measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diam ...
... the stars dwarf the orbit of the Earth.* Riccioli also critiques Landsbergius who cites naked eye measurements of star sizes, including those of Tycho Brahe, that put the observed diameter of first magnitude stars at a minute (60‟‟) or greater, but who then adds that through the telescope star diam ...
POSTERS SESSION I: Atmospheres of Massive Stars
... Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can induce periodic modulations in the surrounding stellar wind and produce observational signatures in line profile ...
... Many classes of these stars are also seen, via photometric or line-profile variability, to pulsate radially or nonradially. It has been suspected for some time that these oscillations can induce periodic modulations in the surrounding stellar wind and produce observational signatures in line profile ...
Early-type stars in the core of the young open cluster Westerlund 2
... is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some weak metallic lines favours an A0 classification, whilst ...
... is dominated by strong and broad H Balmer lines. Weak absorption lines of He λλ 4388, 4471, Mg λ 4481 and Si λ 4552 are also seen. The He λ 4471/Mg λ 4481 intensity ratio indicates a spectral type B8-A0. The appearance of some weak metallic lines favours an A0 classification, whilst ...
Lyra
Lyra (/ˈlaɪərə/; Latin for lyre, from Greek λύρα) is a small constellation. It is one of 48 listed by the 2nd century astronomer Ptolemy, and is one of the 88 constellations recognized by the International Astronomical Union. Lyra was often represented on star maps as a vulture or an eagle carrying a lyre, and hence sometimes referred to as Aquila Cadens or Vultur Cadens. Beginning at the north, Lyra is bordered by Draco, Hercules, Vulpecula, and Cygnus. Lyra is visible from the northern hemisphere from spring through autumn, and nearly overhead, in temperate latitudes, during the summer months. From the southern hemisphere, it is visible low in the northern sky during the winter months.The lucida or brightest star—and one of the brightest stars in the sky—is the white main sequence star Vega, a corner of the Summer Triangle. Beta Lyrae is the prototype of a class of stars known as Beta Lyrae variables, binary stars so close to each other that they become egg-shaped and material flows from one to the other. Epsilon Lyrae, known informally as the Double Double, is a complex multiple star system. Lyra also hosts the Ring Nebula, the second-discovered and best-known planetary nebula.