783 research outputs found
Thermal Structure and Radius Evolution of Irradiated Gas Giant Planets
We consider the thermal structure and radii of strongly irradiated gas giant
planets over a range in mass and irradiating flux. The cooling rate of the
planet is sensitive to the surface boundary condition, which depends on the
detailed manner in which starlight is absorbed and energy redistributed by
fluid motion. We parametrize these effects by imposing an isothermal boundary
condition below the photosphere, and then constrain
from the observed masses and radii. We compute the dependence of
luminosity and core temperature on mass, and core entropy,
finding that simple scalings apply over most of the relevant parameter space.
These scalings yield analytic cooling models which exhibit power-law behavior
in the observable age range , and are confirmed by
time-dependent cooling calculations. We compare our model to the radii of
observed transiting planets, and derive constraints on . Only HD
209458 has a sufficiently accurate radius measurement that is
tightly constrained; the lower error bar on the radii for other planets is
consistent with no irradiation. More accurate radius and age measurements will
allow for a determination of the correlation of with the
equilibrium temperature, informing us about both the greenhouse effect and
day-night asymmetries.Comment: submitted to apj. 14 pages, 20 figure
A Search for Optical Laser Emission from Alpha Centauri AB
A search for laser light from the directions of Alpha Centauri A and B was
performed by examining 15362 optical, high-resolution spectra obtained between
2004 and 2018. None of the spectra exhibit laser emission lines. The threshold
was 10% of the continuum intensity of the spectra of both stars at all
wavelengths between 3850 and 6900 {\AA}. This search would have revealed
optical laser light from the directions of Alpha Cen B if the laser had a power
at least 1.4 to 5.4 MW (depending on wavelength) and was positioned within the
1 arcsecond field of view (projecting to 1.3 AU), for a benchmark 10-meter
laser launcher. For Alpha Cen A, the laser power must be 3 times greater for
detection. Lasers of smaller aperture would also have been detected but would
require more power. Considering all optical surveys, a growing desert is
emerging in the search for extraterrestrial technology.Comment: Dedicated to the late Frank Drak
Observations of magnetic fields on solar-type stars
Magnetic-field observations were carried out for 29 G and K main-sequence stars. The area covering-factors of magnetic regions tends to be greater in the K dwarfs than in the G dwarfs. However, no spectral-type dependence is found for the field strengths, contrary to predictions that pressure equilibrium with the ambient photospheric gas pressure would determine the surface field strengths. Coronal soft X-ray fluxes from the G and K dwarfs correlate well with the fraction of the stellar surface covered by magnetic regions. The dependence of coronal soft X-ray fluxes on photospheric field strengths is consistent with Stein's predicted generation-rates for Alfven waves. These dependences are inconsistent with the one dynamo model for which a specific prediction is offered. Finally, time variability of magnetic fields is seen on the two active stars that have been extensively monitored. Significant changes in magnetic fields are seen to occur on timescales as short as one day
Ca II H and K Chromospheric Emission Lines in Late K and M Dwarfs
We have measured the profiles of the Ca II H and K chromospheric emission
lines in 147 main sequence stars of spectral type M5-K7 (0.30-0.55 solar
masses) using multiple high resolution spectra obtained during six years with
the HIRES spectrometer on the Keck 1 telescope. Remarkably, the average FWHM,
equivalent widths, and line luminosities of Ca II H and K increase by a factor
of 3 with increasing stellar mass over this small range of stellar masses. We
fit the H and K lines with a double Gaussian model to represent both the
chromospheric emission and the non-LTE central absorption. Most of the sample
stars display a central absorption that is typically redshifted by ~0.1 km/s
relative to the emission, but the nature of this velocity gradient remains
unknown. The FWHM of the H and K lines increase with stellar luminosity,
reminiscent of the Wilson-Bappu effect in FGK-type stars. Both the equivalent
widths and FWHM exhibit modest temporal variability in individual stars. At a
given value of M_v, stars exhibit a spread in both the equivalent width and
FWHM of Ca II H and K, due both to a spread in fundamental stellar parameters
including rotation rate, age, and possibly metallicity, and to the spread in
stellar mass at a given M_v. The K line is consistently wider than the H line,
as expected, and its central absorption is more redshifted, indicating that the
H and K lines form at slightly different heights in the chromosphere where the
velocities are slightly different. The equivalent width of H-alpha correlates
with Ca II H and K only for stars having Ca II equivalent widths above ~2
angstroms, suggesting the existence of a magnetic threshold above which the
lower and upper chromospheres become thermally coupled.Comment: 40 pages including 12 figures and 17 pages of tables, accepted for
publication in PAS
Dust in the 55 Cancri planetary system
The presence of debris disks around 1-Gyr-old main sequence stars suggests that an appreciable amount of dust may persist even in mature planetary systems. Here we report the detection of dust emission from 55 Cancri, a star with one, or possibly two, planetary companions detected through radial velocity measurements. Our observations at 850m and 450m imply a dust mass of 0.0008-0.005 Earth masses, somewhat higher than that in the the Kuiper Belt of our solar system. The estimated temperature of the dust grains and a simple model fit both indicate a central disk hole of at least 10 AU in radius. Thus, the region where the planets are detected is likely to be significantly depleted of dust. Our results suggest that far-infrared and sub-millimeter observations are powerful tools for probing the outer regions of extrasolar planetary systems
Dust in the 55 Cancri planetary system
The presence of debris disks around 1-Gyr-old main sequence stars
suggests that an appreciable amount of dust may persist even in mature
planetary systems. Here we report the detection of dust emission from 55
Cancri, a star with one, or possibly two, planetary companions detected through
radial velocity measurements. Our observations at 850m and 450m imply
a dust mass of 0.0008-0.005 Earth masses, somewhat higher than that in the the
Kuiper Belt of our solar system. The estimated temperature of the dust grains
and a simple model fit both indicate a central disk hole of at least 10 AU in
radius. Thus, the region where the planets are detected is likely to be
significantly depleted of dust. Our results suggest that far-infrared and
sub-millimeter observations are powerful tools for probing the outer regions of
extrasolar planetary systems.Comment: 8 pages and 2 figures, to appear in the Astrophysical Journa
KH 15D: A Spectroscopic Binary
We present the results of a high-resolution spectroscopic monitoring program
of the eclipsing pre-main-sequence star KH 15D that reveal it to be a
single-line spectroscopic binary. We find that the best-fit Keplerian model has
a period P = 48.38 days, which is nearly identical to the photometric period.
Thus, we find the best explanation for the periodic dimming of KH 15D is that
the binary motion carries the currently visible star alternately above and
below the edge of an obscuring cloud. The data are consistent with the models
involving an inclined circumstellar disk, as recently proposed by Winn et al.
(2004) and Chiang & Murray-Clay (2004). We show that the mass ratio expected
from models of PMS evolution, together with the mass constraints for the
visible star, restrict the orbital eccentricity to 0.68 < e < 0.80 and the mass
function to 0.125 < Fm < 0.5 Msun.Comment: 8 pages, 4 figures, 3 tables, accepted for publication in September
AJ. Discussion of rotational velocity deferred to Hamilton, et al. (2004, in
prep). Previously reported vsini value in error; Replaced Table 3 with new
Figure 3; Added new Table 2 showing individual radial velocities w.r.t. each
reference star; Fixed typo in Figure
HAT-P-4b: A metal-rich low-density transiting hot Jupiter
We describe the discovery of HAT-P-4b, a low-density extrasolar planet
transiting BD+36 2593, a V = 11.2 mag slightly evolved metal-rich late F star.
The planet's orbital period is 3.056536+/-0.000057 d with a mid-transit epoch
of 2,454,245.8154 +/- 0.0003 (HJD). Based on high-precision photometric and
spectroscopic data, and by using transit light curve modeling, spectrum
analysis and evolutionary models, we derive the following planet parameters:
Mp= 0.68 +/- 0.04 MJ, Rp= 1.27 +/- 0.05 RJ, rho = 0.41 +/- 0.06 g cm-3 and a =
0.0446 +/- 0.0012 AU. Because of its relatively large radius, together with its
assumed high metallicity of that of its parent star, this planet adds to the
theoretical challenges to explain inflated extrasolar planets.Comment: 5 pages, accepted for publication in ApJ
Planetary Companions Around Two Solar Type Stars: HD 195019 and HD 217107
We have enlarged the sample of stars in the planet search at Lick
Observatory. Doppler measurements of 82 new stars observed at Lick Observatory,
with additional velocities from Keck Observatory, have revealed two new planet
candidates.
The G3V/IV star, HD 195019, exhibits Keplerian velocity variations with a
period of 18.27 d, an orbital eccentricity of 0.03 +/- 0.03, and M sin i = 3.51
M_Jup. Based on a measurement of Ca II H&K emission, this star is
chromospherically inactive. We estimate the metallicity of HD 195019 to be
approximately solar from ubvy photometry.
The second planet candidate was detected around HD 217107, a G7V star. This
star exhibits a 7.12 d Keplerian period with eccentricity 0.14 +/- 0.05 and M
sin i = 1.27 M_Jup. HD 217107 is also chromospherically inactive. The
photometric metallicity is found to be [Fe/H] = +0.29 +/- 0.1 dex. Given the
relatively short orbital period, the absence of tidal spin-up of HD 217107
provides a theoretical constraint on the upper limit of the companion mass of <
11 M_Jup.Comment: 15 pages, plus 6 figures. To appear in Jan 1999 PAS
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