John Clare

Kővesi, Simon

doi:10.1057/978-1-349-59183-1

Cited by 22 publications

(2 citation statements)

References 0 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The location of the Sun is marked as a white star and the GC is at (0,0). The maps are displayed using the colormap bgyw from the colorcet package (Kovesi 2015). in the disk. The SA50 model has half of the injected CR luminosity distributed as the SA0 density and the other half distributed as the spiral arms for the R12 ISRF model.…”

Section: Implications For Propagation Throughoutmentioning

confidence: 99%

Cosmic-Ray Propagation in Light of the Recent Observation of Geminga

Jóhannesson

Porter

Moskalenko

2019

ApJ

View full text Add to dashboard Cite

The High Altitude Water Cherenkov (HAWC) telescope recently observed extended emission around the Geminga and PSR B0656+14 pulsar wind nebulae (PWNe). These observations have been used to estimate cosmic-ray (CR) diffusion coefficients near the PWNe that appear to be more than two orders of magnitude smaller than that typically derived for the interstellar medium from the measured abundances of secondary species in CRs. Two-zone diffusion models have been proposed as a solution to this discrepancy, where the slower diffusion zone (SDZ) is confined to a small region around the PWN. Such models are shown to successfully reproduce the HAWC observations of the Geminga PWN while retaining consistency with other CR data. It is found that the size of the SDZ influences the predicted positron flux and the spectral shape of the extended γ-ray emission at lower energies that can be observed with the Fermi Large Area Telescope (Fermi-LAT). If the two observed PWNe are not unique, then it is likely that there are similar pockets of slow diffusion around many CR sources elsewhere in the Milky Way. The consequences of such picture for Galactic CR propagation is explored.

show abstract

Section: Implications For Propagation Throughoutmentioning

confidence: 99%

Cosmic-Ray Propagation in Light of the Recent Observation of Geminga

Jóhannesson

Porter

Moskalenko

2019

ApJ

View full text Add to dashboard Cite

show abstract

“…These GCMs allow for analysis of the effects of various properties of the planetary system on the evolution of climate (e.g. O'Gorman & Schneider 2008;Wolf & Toon 2013, 2015. Such models have also been developed for other terrestrial planets in the Solar System, particularly Venus and Mars (e.g.…”

Section: Introductionmentioning

confidence: 99%

Aquaplanet Models on Eccentric Orbits: Effects of the Rotation Rate on Observables

Adams

Boos

Wolf

2019

View full text Add to dashboard Cite

Rotation and orbital eccentricity both strongly influence planetary climate. Eccentricities can often be measured for exoplanets, but rotation rates are currently difficult or impossible to constrain. Here we examine how the combined effects of rotation and eccentricity on observed emission from ocean-rich terrestrial planets can be used to infer their rotation rates in circumstances where their eccentricities are known. We employ an Earth climate model with no land and a slab ocean, and consider two eccentricities (e = 0.3 and 0.6) and two rotation rates: a fast Earth-like period of 24 hours, and a slower pseudo-synchronous period that generalizes spin synchronization for eccentric orbits. We adopt bandpasses of the Mid-Infrared Instrument on the James Webb Space Telescope as a template for future photometry. At e = 0.3 the rotation rates can be distinguished if the planet transits near periastron, because slow rotation produces a strong day-night contrast and thus an emission minimum during periastron. However, light curves behave similarly if the planet is eclipsed near periastron, as well as for either viewing geometry at e = 0.6. Rotation rates can nevertheless be distinguished using ratios of emission in different bands, one in the water vapor window with another in a region of strong water absorption. These ratios vary over an orbit by 0.1 dex for Earth-like rotation, but by 0.3-0.5 dex for pseudo-synchronous rotation because of large day-night contrast in upper-tropospheric water. For planets with condensible atmospheric constituents in eccentric orbits, rotation regimes might thus be distinguished with infrared observations for a range of viewing geometries. significantly different time scales, operate largely independently of each other. Additionally, Earth's nearly circular orbit means that variations in the Earth-Sun distance are small; Earth's seasons are driven primarily by obliquity rather than eccentricity. Differences in orbital eccentricity, planetary rotation rate, and axial tilt can all have large consequences for atmospheric heating rates and planetary climate. Here we examine how rotation rate and orbital eccentricity control, via the global atmospheric circulation, the radiative properties of a planet's surface and atmosphere. By using detailed representations of the circulation and radiative transfer, we wish to explore whether the rough scale of rotation

show abstract

Clare’s Late Styles

Hodgson

2020

The Lost Romantics

View full text Add to dashboard Cite

John Clare

Cited by 22 publications

References 0 publications

Cosmic-Ray Propagation in Light of the Recent Observation of Geminga

Cosmic-Ray Propagation in Light of the Recent Observation of Geminga

Aquaplanet Models on Eccentric Orbits: Effects of the Rotation Rate on Observables

Clare’s Late Styles

Contact Info

Product

Resources

About