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Brian P. Schmidt - One of the best experts on this subject based on the ideXlab platform.
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A Nearly Polar Orbit for the Extrasolar Hot Jupiter WASP-79b
The Astrophysical Journal, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:We report the measurement of a spin-Orbit misalignment for WASP-79b, a recently discovered, bloated transiting hot Jupiter from the WASP survey. Data were obtained using the CYCLOPS2 optical-fiber bundle and its simultaneous calibration system feeding the UCLES spectrograph on the Anglo-Australian Telescope. We have used the Rossiter-McLaughlin effect to determine the sky-projected spin-Orbit angle to be lambda = -106+19-13 degrees. This result indicates a significant misalignment between the spin axis of the host star and the Orbital plane of the planet -- the planet being in a nearly Polar Orbit. WASP-79 is consistent with other stars that have Teff > 6250K and host hot Jupiters in spin-Orbit misalignment.
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A Nearly Polar Orbit for the Extrasolar Hot Jupiter WASP-79b
The Astrophysical Journal, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:We report the measurement of a spin-Orbit misalignment for WASP-79b, a recently discovered, bloated hot Jupiter from the Wide Angle Search for Planets (WASP) survey. Data were obtained using the CYCLOPS2 optical-fiber bundle and its simultaneous calibration system feeding the UCLES spectrograph on the Anglo-Australian Telescope. We have used the Rossiter-McLaughlin effect to determine the sky-projected spin-Orbit angle to be . This result indicates a significant misalignment between the spin axis of the host star and the Orbital plane of the planet?the planet being in a nearly Polar Orbit. WASP-79 is consistent with other stars that have T eff > 6250?K and host hot Jupiters in spin-Orbit misalignment.
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A hot jupiter in a nearly Polar Orbit
Proceedings of the International Astronomical Union, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:AbstractWe measured the spin-Orbit misalignment for WASP-79b, a transiting hot Jupiter from the WASP survey. Using the Rossiter-McLaughlin effect during the transit event, we determined the sky-projected obliquity to be λ = −106+10−8○. This result indicates that the planet is in a nearly Polar Orbit.
R. J. Forsyth - One of the best experts on this subject based on the ideXlab platform.
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stream interaction regions at high heliographic latitudes during ulysses second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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Stream Interaction Regions at High Heliographic Latitudes During Ulysses12/22/2004 6:25PM Second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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stream interaction regions at high heliographic latitudes during ulysses12 22 2004 6 25pm second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, D J Mccomas, R M Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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Stream Interaction Regions at High Heliographic Latitudes during Ulysses ’ Second Polar Orbit
The 3-D Heliosphere at Solar Maximum, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
J. T. Gosling - One of the best experts on this subject based on the ideXlab platform.
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stream interaction regions at high heliographic latitudes during ulysses second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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Stream Interaction Regions at High Heliographic Latitudes During Ulysses12/22/2004 6:25PM Second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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stream interaction regions at high heliographic latitudes during ulysses12 22 2004 6 25pm second Polar Orbit
Space Science Reviews, 2001Co-Authors: J. T. Gosling, D J Mccomas, R M Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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Stream Interaction Regions at High Heliographic Latitudes during Ulysses ’ Second Polar Orbit
The 3-D Heliosphere at Solar Maximum, 2001Co-Authors: J. T. Gosling, David J. Mccomas, Ruth M. Skoug, R. J. ForsythAbstract:Ulysses observed well-defined stream interaction regions, SIRs, associated with solar wind stream structure up to a latitude of S65° and shocks to at least a latitude of S71° during the second Polar Orbit. These SIRs and shocks produced a substantial heliospheric processing of the solar wind. Only a subset of the SIRs recurred on successive solar rotations and only about half of the well-defined SIRs observed poleward of S9.8° were bounded by forward-reverse shock pairs. The majority of the SIRs had local magnetic topologies and azimuthal orientations similar to, but meridional tilts different from, those observed in the first Polar Orbit when most SIRs corotated with the Sun. The irregular meridional tilts presumably were a consequence of a complex coronal geometry and the temporally evolving nature of the solar wind flow at this time. A lack of reverse shocks poleward of S54° (with one exception) and a lack of well defined SIRs poleward of S65° is evidence that SIRs develop more slowly with distance at high latitudes.
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solar wind observations over ulysses first full Polar Orbit
Journal of Geophysical Research, 2000Co-Authors: D J Mccomas, J. T. Gosling, B L Barraclough, H O Funsten, E Santiagomunoz, R M Skoug, B E Goldstein, M Neugebauer, P Riley, A BaloghAbstract:This study examines solar wind plasma and magnetic field observations from Ulysses' first full Polar Orbit in order to characterize the high-latitude solar wind under conditions of decreasing and low solar activity. By comparing observations taken over nearly all heliolatitudes and two different intervals covering the same radial distances, we are able to separate the radial and latitudinal variations in the solar wind. We find that once the radial gradients are removed, none of the high-latitude solar wind parameters show much latitudinal variation, indicating that the solar wind emanating from the Polar coronal holes is extremely uniform. In addition, by examining nearly 6 years of data starting in the declining phase of the last solar cycle and extending through the most recent solar minimum, we are able to address hemispheric asymmetries in the observations. We find that these asymmetries are most likely driven by differences in the solar wind source over the solar cycle and indicate that more energy goes into the Polar solar wind during the declining phase of the solar cycle than around minimum. Because the mass flux is larger in the declining phase while the speeds are very similar, we conclude that this energy is introduced at an altitude below the solar wind acceleration critical point. Finally, we provide details of the statistics of over 20 solar wind parameters so that upcoming observations from Ulysses' second Polar Orbit, during much more active times on the Sun, can be readily compared to the quieter first Orbit results.
B. C. Addison - One of the best experts on this subject based on the ideXlab platform.
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A Nearly Polar Orbit for the Extrasolar Hot Jupiter WASP-79b
The Astrophysical Journal, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:We report the measurement of a spin-Orbit misalignment for WASP-79b, a recently discovered, bloated transiting hot Jupiter from the WASP survey. Data were obtained using the CYCLOPS2 optical-fiber bundle and its simultaneous calibration system feeding the UCLES spectrograph on the Anglo-Australian Telescope. We have used the Rossiter-McLaughlin effect to determine the sky-projected spin-Orbit angle to be lambda = -106+19-13 degrees. This result indicates a significant misalignment between the spin axis of the host star and the Orbital plane of the planet -- the planet being in a nearly Polar Orbit. WASP-79 is consistent with other stars that have Teff > 6250K and host hot Jupiters in spin-Orbit misalignment.
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A Nearly Polar Orbit for the Extrasolar Hot Jupiter WASP-79b
The Astrophysical Journal, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:We report the measurement of a spin-Orbit misalignment for WASP-79b, a recently discovered, bloated hot Jupiter from the Wide Angle Search for Planets (WASP) survey. Data were obtained using the CYCLOPS2 optical-fiber bundle and its simultaneous calibration system feeding the UCLES spectrograph on the Anglo-Australian Telescope. We have used the Rossiter-McLaughlin effect to determine the sky-projected spin-Orbit angle to be . This result indicates a significant misalignment between the spin axis of the host star and the Orbital plane of the planet?the planet being in a nearly Polar Orbit. WASP-79 is consistent with other stars that have T eff > 6250?K and host hot Jupiters in spin-Orbit misalignment.
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A hot jupiter in a nearly Polar Orbit
Proceedings of the International Astronomical Union, 2013Co-Authors: B. C. Addison, C. G. Tinney, Duncan J. Wright, Daniel Bayliss, George Zhou, Joel D. Hartman, Gáspár Á. Bakos, Brian P. SchmidtAbstract:AbstractWe measured the spin-Orbit misalignment for WASP-79b, a transiting hot Jupiter from the WASP survey. Using the Rossiter-McLaughlin effect during the transit event, we determined the sky-projected obliquity to be λ = −106+10−8○. This result indicates that the planet is in a nearly Polar Orbit.
Howard Isaacson - One of the best experts on this subject based on the ideXlab platform.
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the tess keck survey iv a retrograde Polar Orbit for the ultra low density hot super neptune wasp 107b
arXiv: Earth and Planetary Astrophysics, 2021Co-Authors: Ryan A Rubenzahl, Andrew W Howard, Howard Isaacson, Fei Dai, Ashley Chontos, Steven Giacalone, Jack Lubin, Lee Rosenthal, Natalie M BatalhaAbstract:We measured the Rossiter-McLaughlin effect of WASP-107b during a single transit with Keck/HIRES. We found the sky-projected inclination of WASP-107b's Orbit, relative to its host star's rotation axis, to be $|\lambda| = {118}^{+38}_{-19}$ degrees. This confirms the misaligned/Polar Orbit that was previously suggested from spot-crossing events and adds WASP-107b to the growing population of hot Neptunes in Polar Orbits around cool stars. WASP-107b is also the fourth such planet to have a known distant planetary companion. We examined several dynamical pathways by which this companion could have induced such an obliquity in WASP-107b. We find that nodal precession and disk dispersal-driven tilting can both explain the current Orbital geometry while Kozai-Lidov cycles are suppressed by general relativity. While each hypothesis requires a mutual inclination between the two planets, nodal precession requires a much larger angle which for WASP-107 is on the threshold of detectability with future Gaia astrometric data. As nodal precession has no stellar type dependence, but disk dispersal-driven tilting does, distinguishing between these two models is best done on the population level. Finding and characterizing more extrasolar systems like WASP-107 will additionally help distinguish whether the distribution of hot-Neptune obliquities is a dichotomy of aligned and Polar Orbits or if we are uniformly sampling obliquities during nodal precession cycles.
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kepler 63b a giant planet in a Polar Orbit around a young sun like star
The Astrophysical Journal, 2013Co-Authors: Roberto Sanchisojeda, Joshua N Winn, Geoffrey W Marcy, Andrew W Howard, Howard Isaacson, John Asher Johnson, Guillermo Torres, Simon Albrecht, T L CampanteAbstract:We present the discovery and characterization of a giant planet Orbiting the young Sun-like star Kepler-63 (KOI-63, m_(Kp) = 11.6, T_(eff) = 5576 K, M_★ = 0.98 M_☉). The planet transits every 9.43 days, with apparent depth variations and brightening anomalies caused by large starspots. The planet's radius is 6.1 ± 0.2 R_⊕, based on the transit light curve and the estimated stellar parameters. The planet's mass could not be measured with the existing radial-velocity data, due to the high level of stellar activity, but if we assume a circular Orbit, then we can place a rough upper bound of 120 M_⊕ (3σ). The host star has a high obliquity (ψ = 104°), based on the Rossiter-McLaughlin effect and an analysis of starspot-crossing events. This result is valuable because almost all previous obliquity measurements are for stars with more massive planets and shorter-period Orbits. In addition, the Polar Orbit of the planet combined with an analysis of spot-crossing events reveals a large and persistent Polar starspot. Such spots have previously been inferred using Doppler tomography, and predicted in simulations of magnetic activity of young Sun-like stars.
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kepler 63b a giant planet in a Polar Orbit around a young sun like star
arXiv: Earth and Planetary Astrophysics, 2013Co-Authors: Roberto Sanchisojeda, Joshua N Winn, Geoffrey W Marcy, Andrew W Howard, Howard Isaacson, John Asher Johnson, Guillermo Torres, Simon Albrecht, T L CampanteAbstract:We present the discovery and characterization of a giant planet Orbiting the young Sun-like star Kepler-63 (KOI-63, $m_{\rm Kp} = 11.6$, $T_{\rm eff} = 5576$ K, $M_\star = 0.98\, M_\odot$). The planet transits every 9.43 days, with apparent depth variations and brightening anomalies caused by large starspots. The planet's radius is $6.1 \pm 0.2 R_{\earth}$, based on the transit light curve and the estimated stellar parameters. The planet's mass could not be measured with the existing radial-velocity data, due to the high level of stellar activity, but if we assume a circular Orbit we can place a rough upper bound of $120 M_{\earth}$ (3$\sigma$). The host star has a high obliquity ($\psi$ = $104^{\circ}$), based on the Rossiter-McLaughlin effect and an analysis of starspot-crossing events. This result is valuable because almost all previous obliquity measurements are for stars with more massive planets and shorter-period Orbits. In addition, the Polar Orbit of the planet combined with an analysis of spot-crossing events reveals a large and persistent Polar starspot. Such spots have previously been inferred using Doppler tomography, and predicted in simulations of magnetic activity of young Sun-like stars.
