The Organic Refractory Material in the Diffuse Interstellar Medium
... through a program of study in which several sight lines through the DISM were compared (Sandford et al. 1991, Pendleton et al. 1994, and Whittet 1997). The proÐles and band positions agree in cases where various types of stars are seen through intervening dust along di†erent directions from the Eart ...
... through a program of study in which several sight lines through the DISM were compared (Sandford et al. 1991, Pendleton et al. 1994, and Whittet 1997). The proÐles and band positions agree in cases where various types of stars are seen through intervening dust along di†erent directions from the Eart ...
A search for the cause of cyclical wind variability in O stars
... Hα line profiles. The epochs of maximum absorption in the UV resonance lines due to discrete absorption components (DACs) coincide in phase with the maxima in blue-shifted Hα absorption. This implies that the periodic variability originates close to the stellar surface. The phase−velocity relation s ...
... Hα line profiles. The epochs of maximum absorption in the UV resonance lines due to discrete absorption components (DACs) coincide in phase with the maxima in blue-shifted Hα absorption. This implies that the periodic variability originates close to the stellar surface. The phase−velocity relation s ...
Properties of Galactic B supergiants
... early to mid B supergiants (Vink et al. 2000). In addition, CNO abundances are readily obtained from optical spectroscopy, for comparison to evolutionary model predictions. Notably, Trundle et al. (2004) and Trundle & Lennon (2005) have studied a large sample of SMC B supergiants using the line blan ...
... early to mid B supergiants (Vink et al. 2000). In addition, CNO abundances are readily obtained from optical spectroscopy, for comparison to evolutionary model predictions. Notably, Trundle et al. (2004) and Trundle & Lennon (2005) have studied a large sample of SMC B supergiants using the line blan ...
90377 Sedna
... again for 12,000 years. Although Sedna is listed on NASA’s Solar System exploration website,[65] NASA is not known to be considering any type of mission at this time.[66] It was calculated that a flyby mission to Sedna could take 24.48 years using a Jupiter gravity assist, based on launch dates of 6 ...
... again for 12,000 years. Although Sedna is listed on NASA’s Solar System exploration website,[65] NASA is not known to be considering any type of mission at this time.[66] It was calculated that a flyby mission to Sedna could take 24.48 years using a Jupiter gravity assist, based on launch dates of 6 ...
The Solar Tachocline: A Self-Consistent Model of Magnetic
... high pressure and temperature cause hydrogen nuclei to fuse into helium, releasing the energy that powers the Sun (and all life on Earth). The thermal energy released in the core is carried outward by photon radiation. Throughout the solar interior, pressure, density and temperature all decrease out ...
... high pressure and temperature cause hydrogen nuclei to fuse into helium, releasing the energy that powers the Sun (and all life on Earth). The thermal energy released in the core is carried outward by photon radiation. Throughout the solar interior, pressure, density and temperature all decrease out ...
EOS Experts Guide - by topic and by name
... Brief biographies of scientists from the three EOS centers — the Earth Systems Research Center, Ocean Process Analysis Laboratory, and the Space Science Center — provide areas of specialty, research interests, credentials, and contact information. Experts can also be found by means of an alphabetica ...
... Brief biographies of scientists from the three EOS centers — the Earth Systems Research Center, Ocean Process Analysis Laboratory, and the Space Science Center — provide areas of specialty, research interests, credentials, and contact information. Experts can also be found by means of an alphabetica ...
Comets
... The ejected material made the comet brighter, but it dissipated after about two days • We’re waiting to hear about the composition of the comet’s surface and the material ejected by the impact • This comet has an appearance quite different from the other three comets we have examined ...
... The ejected material made the comet brighter, but it dissipated after about two days • We’re waiting to hear about the composition of the comet’s surface and the material ejected by the impact • This comet has an appearance quite different from the other three comets we have examined ...
Solar Radiation - Energy
... range of frequencies and wavelengths. Nevertheless, not all bodies emit light. Actually, most visible objects we do not perceive because of the radiation they emit but because of the light they reflect and that originates from other sources. We know this because at night we cannot see the majority o ...
... range of frequencies and wavelengths. Nevertheless, not all bodies emit light. Actually, most visible objects we do not perceive because of the radiation they emit but because of the light they reflect and that originates from other sources. We know this because at night we cannot see the majority o ...
Uranus
... on other planets—that is, the Sun doesn't rise and set like on other planets. The cause for this highly unusual axial tilt is theorized to be the effect of a large body striking Uranus with such force that it essentially knocked the planet over on its side. ...
... on other planets—that is, the Sun doesn't rise and set like on other planets. The cause for this highly unusual axial tilt is theorized to be the effect of a large body striking Uranus with such force that it essentially knocked the planet over on its side. ...
SOFT X-RAY EMISSIONS FROM PLANETS, MOONS, AND COMETS
... These results invalidate the idea that Jovian auroral x-ray emissions are mainly excited by steady precipitation of heavy energetic ions from the inner magnetosphere [cf. Ref. 2]. Instead, the x-rays seem to result from currently unexplained processes in the outer magnetosphere that produce highly l ...
... These results invalidate the idea that Jovian auroral x-ray emissions are mainly excited by steady precipitation of heavy energetic ions from the inner magnetosphere [cf. Ref. 2]. Instead, the x-rays seem to result from currently unexplained processes in the outer magnetosphere that produce highly l ...
The Exploration of Neptune and Triton
... surface revealed a young surface containing landforms unlike any others seen in the solar system including “cantaloupe terrain”, active “geysers”, and long linear features which may be similar to Europa’s double ridges (Prockter et al., 2006). Many of Triton’s surface features may be cryovolcanic in ...
... surface revealed a young surface containing landforms unlike any others seen in the solar system including “cantaloupe terrain”, active “geysers”, and long linear features which may be similar to Europa’s double ridges (Prockter et al., 2006). Many of Triton’s surface features may be cryovolcanic in ...
Geosystems, 7e (Christopherson) Chapter 2 Solar Energy to Earth
... 67) Which of the following is true of the number of hours of daylight? A) The number of hours of daylight includes the hours between dawn and twilight, not just the hours from sunrise to sunset. B) The number of hours of daylight varies depending on the latitude of the observer. C) The number of hou ...
... 67) Which of the following is true of the number of hours of daylight? A) The number of hours of daylight includes the hours between dawn and twilight, not just the hours from sunrise to sunset. B) The number of hours of daylight varies depending on the latitude of the observer. C) The number of hou ...
DYNAMICAL EVOLUTION OF THE OORT CLOUD Paul R
... It was found that 23% of the stars failed to survive for ten orbits, the estimated number of observed cycles of extinction in the fossil record. Most of those lost diffused to aphelia beyond the sun's sphere of influence, a likely result considering the large initial aphelion. Continuing the integra ...
... It was found that 23% of the stars failed to survive for ten orbits, the estimated number of observed cycles of extinction in the fossil record. Most of those lost diffused to aphelia beyond the sun's sphere of influence, a likely result considering the large initial aphelion. Continuing the integra ...
The magnetic field and wind confinement of b Cephei: new clues for
... the sum of the logarithmic mass-loss rate (expressed in M( yr21) and the logarithmic C IV ionization fraction should equal about 212. Assuming a logarithmic C IV ionization fraction of 23 (typical for O and early B stars), we obtain a mass-loss rate of about 1029 M( yr21. Given the rather poor accur ...
... the sum of the logarithmic mass-loss rate (expressed in M( yr21) and the logarithmic C IV ionization fraction should equal about 212. Assuming a logarithmic C IV ionization fraction of 23 (typical for O and early B stars), we obtain a mass-loss rate of about 1029 M( yr21. Given the rather poor accur ...
Astronomy Astrophysics
... young solar analogues. The sample includes five single G0-G5V stars with ages between '130 Myr and 700 Myr: EK Dra, π1 UMa, HN Peg, k1 Cet and BE Cet. In this study we also include the Pleiades-age ('130 Myr) K0V star DX Leo. Our analysis is based on high precision photometric observations carried o ...
... young solar analogues. The sample includes five single G0-G5V stars with ages between '130 Myr and 700 Myr: EK Dra, π1 UMa, HN Peg, k1 Cet and BE Cet. In this study we also include the Pleiades-age ('130 Myr) K0V star DX Leo. Our analysis is based on high precision photometric observations carried o ...
Magneto-thermal Disk Wind from Protoplanetary Disks
... well known that the wind properties depend mainly on the strength and distribution of the magnetic flux threading the disk, and on the mass loading, with the latter mainly controlled by disk physics and thermodynamics. In this paper, we focus on MHD disk winds from very weakly ionized protoplanetary ...
... well known that the wind properties depend mainly on the strength and distribution of the magnetic flux threading the disk, and on the mass loading, with the latter mainly controlled by disk physics and thermodynamics. In this paper, we focus on MHD disk winds from very weakly ionized protoplanetary ...
Stellar Wind Mechanisms and Instabilities
... the realization that nearly all stars lose mass through a more or less continuous surface outflow called a “stellar wind”. While it was long apparent that stars could eject material in dramatic outburts like novae or supernovae, the concept of continuous mass loss in the relatively quiescent phases ...
... the realization that nearly all stars lose mass through a more or less continuous surface outflow called a “stellar wind”. While it was long apparent that stars could eject material in dramatic outburts like novae or supernovae, the concept of continuous mass loss in the relatively quiescent phases ...
Full Paper - PDF - Armagh Observatory
... Neptune, first for a total mass in the annulus of 0.33 M and then for 0.1 M . These calculations yielded figures of 200 million and 2000 million objects with individual masses of about 2 × 10–9 M and 5 × 10 –11 M , respectively, i.e., they would be smaller and more numerous than most of the then-kno ...
... Neptune, first for a total mass in the annulus of 0.33 M and then for 0.1 M . These calculations yielded figures of 200 million and 2000 million objects with individual masses of about 2 × 10–9 M and 5 × 10 –11 M , respectively, i.e., they would be smaller and more numerous than most of the then-kno ...
On some properties of coronal mass ejections in solar cycle 23
... maximum. On one day during solar maximum, 13 CMEs were recorded by SOHO; there were several days with more than 10 CMEs (Gopalswamy et al. 20003a). The daily CME rate averaged over Carrington Rotation (27.3 days), increases from less than 1 during solar minimum in 1996 to slightly more than 6 during ...
... maximum. On one day during solar maximum, 13 CMEs were recorded by SOHO; there were several days with more than 10 CMEs (Gopalswamy et al. 20003a). The daily CME rate averaged over Carrington Rotation (27.3 days), increases from less than 1 during solar minimum in 1996 to slightly more than 6 during ...
and galaxies
... regions of galaxy.Gas/dust in disk absorbs visible light, but 21cm H-I line ok. Thus, radiotelescopes can map velocity and distribution of H-I gas. Galactic bulge. Spheroidal region near centre of galaxy. Only certain w.lengths observed due to dust. Disc meets the galactic bulge at a radius of appro ...
... regions of galaxy.Gas/dust in disk absorbs visible light, but 21cm H-I line ok. Thus, radiotelescopes can map velocity and distribution of H-I gas. Galactic bulge. Spheroidal region near centre of galaxy. Only certain w.lengths observed due to dust. Disc meets the galactic bulge at a radius of appro ...
8th International Workshop on Planetary, Solar and Heliospheric
... recommend that you take your jacket/coat with you since there is no heating in the wine cellar. This event is sponsored by the Space Research Institute of the Austrian Academy of Sciences. Our second social event is a visit to the chocolate factory “Zotter” in Bergl close to Riegersburg. We will lea ...
... recommend that you take your jacket/coat with you since there is no heating in the wine cellar. This event is sponsored by the Space Research Institute of the Austrian Academy of Sciences. Our second social event is a visit to the chocolate factory “Zotter” in Bergl close to Riegersburg. We will lea ...
Links Between Pulsation and Line-Driven Mass Loss in Massive Stars
... winds also often show modulation at periods comparable to the stellar rotation period. July 30, 2001 ...
... winds also often show modulation at periods comparable to the stellar rotation period. July 30, 2001 ...
Foreword You`ll notice here that I hardly make mention of gravity, if
... Nibiru's core magnetic circumference: C = π x 9,799,461 = 30,785,915 km. We see that Nibiru's black magnetic shell represents a protective region with such dense magnetism that it permits no light, visible or invisible, to pass through it, except for the intense radiation from the core. The core, at ...
... Nibiru's core magnetic circumference: C = π x 9,799,461 = 30,785,915 km. We see that Nibiru's black magnetic shell represents a protective region with such dense magnetism that it permits no light, visible or invisible, to pass through it, except for the intense radiation from the core. The core, at ...
Gresham College
... The last return that is still remembered by some people alive today is that of 1910. Although many people did see the comet in the late spring, others swear they saw it earlier. In fact, Halley was upstaged by a much brighter.comet - the Great Daylight Comet - that graced the skies in January and Fe ...
... The last return that is still remembered by some people alive today is that of 1910. Although many people did see the comet in the late spring, others swear they saw it earlier. In fact, Halley was upstaged by a much brighter.comet - the Great Daylight Comet - that graced the skies in January and Fe ...
Comparative Planetology
... solar wind, which generate substorms and geomagnetic storms reflected in perturbations to the magnetic field morphology as well as in the aurora. Jupiter’s magnetosphere appears to be rotationally driven, due to both the rapid rotation of the planet and the internal plasma loading provided by Io. Th ...
... solar wind, which generate substorms and geomagnetic storms reflected in perturbations to the magnetic field morphology as well as in the aurora. Jupiter’s magnetosphere appears to be rotationally driven, due to both the rapid rotation of the planet and the internal plasma loading provided by Io. Th ...
Heliosphere
The heliosphere is the bubble-like region of space dominated by the Sun, which extends far beyond the orbit of Pluto. Plasma ""blown"" out from the Sun, known as the solar wind, creates and maintains this bubble against the outside pressure of the interstellar medium, the hydrogen and helium gas that permeates the Milky Way Galaxy. The solar wind flows outward from the Sun until encountering the termination shock, where motion slows abruptly. The Voyager spacecraft have actively explored the outer reaches of the heliosphere, passing through the shock and entering the heliosheath, a transitional region which is in turn bounded by the outermost edge of the heliosphere, called the heliopause. The overall shape of the heliosphere is controlled by the interstellar medium, through which it is traveling, as well as the Sun, and does not appear to be perfectly spherical. The limited data available and unexplored nature of these structures have resulted in many theories.On September 12, 2013, NASA announced that Voyager 1 had exited the heliosphere on August 25, 2012, when it measured a sudden increase in plasma density of about forty times. Because the heliopause marks one boundary between the Sun's solar wind and the rest of the galaxy, a spacecraft such as Voyager 1 which has departed the heliosphere can be said to have reached interstellar space.