N. P. Carleton

Center for Astrophysics Harvard & Smithsonian

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Co-Authors

C. Papaliolios

Harvard University

Paul Horowitz

Harvard University

Wesley A. Traub

Jet Propulsion Laboratory

W. A. Traub

Jet Propulsion Laboratory

N. Thureau

University of St Andrews

E. Pedretti

Rutherford Appleton Laboratory

W. A. Traub

Center for Astrophysics Harvard & Smithsonian

S. Lacour

Janssen (France)

P. A. Schuller

University of Cologne

Jean-Philippe Berger

Centre National de la Recherche Scientifique

Cooperative Institutions

Center for Astrophysics Harvard & Smithsonian

Harvard University

California Institute of Technology

Harvard University Press

Smithsonian Astrophysical Observatory

Centre National de la Recherche Scientifique

Jet Propulsion Laboratory

University of California, Berkeley

Laboratoire d’études spatiales et d’instrumentation en astrophysique

Harvard College Observatory

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Excitation of nitrogen by fast protons and electrons

Journal of Geophysical Research Atmospheres (1971)

W. F. Sheridan O. Oldenberg N. P. Carleton

Cross sections are measured for excitation of the (0, 0) first negative band by protons in the range 5000 to 25,000 ev and by electrons in the range 45 to 25,000 ev. Upper limits are given for the very weak proton excitation of the first and second positive systems. To find the cross sections for the primary collisions and to avoid secondary effects, measurements are extrapolated to zero pressure. Not all intensities emitted are proportional to the pressure. The processes responsible for these deviations, excitation by neutral atoms and collisional deactivation, are investigated.

10.1029/ja076i010p02429

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Citations (15)

A search for H2O and Ch4 in Comet Kohoutek

Icarus (1974)

Wesley A. Traub N. P. Carleton

Albedo (alchemy)

Production rate

Geometric albedo

10.1016/0019-1035(74)90024-4

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Citations (5)

Observations of O2, H2O and HD in Planetary Atmospheres

Springer eBooks (1974)

Wesley A. Traub N. P. Carleton

Atmosphere of Jupiter

Line (geometry)

Jupiter (rocket family)

10.1007/978-94-010-2206-4_17

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Citations (20)

The Relation of the Recent Atmospheric Dust Measurements of Volz and Goody to the Problem of Meteoric Influx

Journal of the Atmospheric Sciences (1962)

N. P. Carleton

Atmospheric Dust

10.1175/1520-0469(1962)019<0424:trotra>2.0.co;2

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Citations (5)

Detection of Molecular Oxygen on Mars

Science (1972)

N. P. Carleton Wesley A. Traub

Molecular oxygen was detected in martian spectra near 7635 angstroms and its abundance measured both during and after the 1971 dust storm. Its column abundance in the clear martian atmosphere is about 10.4 +/- 1.0 centimeters amagat, giving a mixing ratio of molecular oxygen to carbon dioxide of 1.3 x 10-(3). The mixing ratio of molecular oxygen to carbon monoxide (1.4 +/- 0.3) is quite different from the value of 0.5 that would result from the photolysis of a pure carbon dioxide atmosphere, which indicates that there is or was a net source of oxygen relative to carbon (probably water) in the martian atmosphere.

Atmosphere of Mars

Carbon fibers

Mixing ratio

10.1126/science.177.4053.988

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Citations (104)

A Summary of the Observations of the Twin QSOs, 0957+561 A,B

Springer eBooks (1980)

Frederic H. Chaffee R. J. Weymann Marc Davis N. P. Carleton D. Walsh

QSOS

10.1007/978-94-009-9040-1_30

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Citations (0)

ENERGY TRANSFER TO AND THROUGH IONOSPHERIC ELECTRONS.

N. P. Carleton

Energy can be transferred through the ionospheric electrons in essentially three ways : (1) the degradation of fast electrons (photoelectrons or precipitated particles), (2) the flow of electric currents, (3) thermal conduction.

Source

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Spectrographic observation of a mid-latitude red auroral arc

Journal of Geophysical Research Atmospheres (1965)

N. P. Carleton J. R. Roach

In recent years Barbier and Roach, with collaborators, have observed, during times of strong magnetic activity, intense (though still invisible) emission of the [O I] red lines, λ 6300–6364 A, well to the equatorward side of active auroral displays. The emission comes from a region between 300 and 500 km in altitude, extending over several hundred kilometers in latitude and several thousand kilometers in longitude. It is, in general, separated from the main body of auroral luminosity, and within it the other prominent auroral and airglow emissions, such as [O I], λ 5577 A; N2+, λ 3914 A; and Na, λ 5893 A, are not measurably enhanced. The emission persists over several hours with sluggish geographical movements and slow changes in intensity, in contrast with the more dynamic and kaleidoscopic nature of visual auroras.

Airglow

Longitude

Low latitude

Intensity

10.1029/jz070i005p01262

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Citations (6)

Spectroscopic Observations of Winds on Venus

Journal of the Atmospheric Sciences (1975)

W. A. Traub N. P. Carleton

We have measured the differential Doppler shift between various points on Venus using a high-resolution PEPSIOS interferometer (three Fabry-Perot etalons in series). Using both a CO2 line and a Fraunhofer line we find a mean zonal wind velocity near the equator of −83 ± 10 m s−1 (retrograde); the velocity appears to vary from about −2 to −125 m s−1, with a time scale of greater than one week. Meridional velocities are measured to be weak (on the order of 30 m s−1 or less). The equatorial zonal velocity appears to be smaller (−73 m s−1) in the “morning” than in the “afternoon” (−111 m s−1) where the times of day are for retrograde rotation. A comparison with reported velocities of the ultraviolet dark markings reveals general agreement in that both find the motion to be retrograde, variable, and accelerated during the day. A new potential source of systematic error in all spectroscopic determinations of the differential Doppler shift of nonuniformly illuminated objects is pointed out.

Line (geometry)

10.1175/1520-0469(1975)032<1045:soowov>2.0.co;2

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Citations (23)

Optical Search for Pulsations from Pulsating Radio Source CP 1919

Science (1968)

C. Papaliolios N. P. Carleton Paul Horowitz W. Liller

Optical observations of the 18th magnitude blue star and of the faint red object in the approximate location of the pulsating radio source CP 1919 disclose no pulsations of visible light, in a mode similar to that of the radio pulsations, of more than 0.4 percent or 0.8 percent, respectively, of the total visible output; or, for a sinusoidal modulation with the same period, no more than a 4-percent, or 8-percent, root-mean-square intensity fluctuation.

Modulation (music)

Root mean square

Star (game theory)

Intensity

10.1126/science.160.3832.1104

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Citations (10)