1,793 research outputs found
The Transit Light Curve Project. VIII. Six Occultations of the Exoplanet TrES-3
We present photometry of the exoplanet host star TrES-3 spanning six
occultations (secondary eclipses) of its giant planet. No flux decrements were
detected, leading to 99%-confidence upper limits on the planet-to-star flux
ratio of 0.00024, 0.0005, and 0.00086 in the i, z, and R bands respectively.
The corresponding upper limits on the planet's geometric albedo are 0.30, 0.62,
and 1.07. The upper limit in the i band rules out the presence of highly
reflective clouds, and is only a factor of 2-3 above the predicted level of
thermal radiation from the planet.Comment: To appear in AJ [14 pages
Using MOST to reveal the secrets of the mischievous Wolf-Rayet binary CV Ser
The WR binary CV Serpentis (= WR113, WC8d + O8-9IV) has been a source of
mystery since it was shown that its atmospheric eclipses change with time over
decades, in addition to its sporadic dust production. The first high-precision
time-dependent photometric observations obtained with the MOST space telescope
in 2009 show two consecutive eclipses over the 29d orbit, with varying depths.
A subsequent MOST run in 2010 showed a seemingly asymmetric eclipse profile. In
order to help make sense of these observations, parallel optical spectroscopy
was obtained from the Mont Megantic Observatory (2009, 2010) and from the
Dominion Astrophysical Observatory (2009). Assuming these depth variations are
entirely due to electron scattering in a beta-law wind, an unprecedented 62%
increase in mass-loss rate is observed over one orbital period. Alternatively,
no change in mass-loss rate would be required if a relatively small fraction of
the carbon ions in the wind globally recombined and coaggulated to form carbon
dust grains. However, it remains a mystery as to how this could occur. There
also seems to be evidence for the presence of corotating interaction regions
(CIR) in the WR wind: a CIR-like signature is found in the light curves,
implying a potential rotation period for the WR star of 1.6 d. Finally, a new
circular orbit is derived, along with constraints for the wind collision.Comment: 11 pages, 11 figures, 5 table
A stable quasi-periodic 4.18 d oscillation and mysterious occultations in the 2011 MOST light curve of TWHya
We present an analysis of the 2011 photometric observations of TW Hya by the
MOST satellite; this is the fourth continuous series of this type. The
large-scale light variations are dominated by a strong, quasi-periodic 4.18 d
oscillation with superimposed, apparently chaotic flaring activity; the former
is most likely produced by stellar rotation with one large hot spot created by
a stable accretion funnel in the stable regime of accretion while the latter
may be produced by small hot spots, created at moderate latitudes by unstable
accretion tongues. A new, previously unnoticed feature is a series of
semi-periodic, well defined brightness dips of unknown nature of which 19 were
observed during 43 days of our nearly-continuous observations. Re-analysis of
the 2009 MOST light curve revealed the presence of 3 similar dips. On the basis
of recent theoretical results, we tentatively conclude that the dips may
represent occultations of the small hot spots created by unstable accretion
tongues by hypothetical optically thick clumps.Comment: Printed in MNRA
Non-detection of previously reported transits of HD 97658b with MOST photometry
The radial velocity-discovered exoplanet HD 97658b was recently announced to
transit, with a derived planetary radius of 2.93 \pm 0.28 R_{Earth}. As a
transiting super-Earth orbiting a bright star, this planet would make an
attractive candidate for additional observations, including studies of its
atmospheric properties. We present and analyze follow-up photometric
observations of the HD 97658 system acquired with the MOST space telescope. Our
results show no transit with the depth and ephemeris reported in the
announcement paper. For the same ephemeris, we rule out transits for a planet
with radius larger than 2.09 R_{Earth}, corresponding to the reported 3\sigma
lower limit. We also report new radial velocity measurements which continue to
support the existence of an exoplanet with a period of 9.5 days, and obtain
improved orbital parameters.Comment: 16 pages, 4 figures; 1 Table; accepted for publication in ApJL,
includes changes made in response to the referee repor
Photometric variability in FU Ori and Z CMa as observed by MOST
Photometric observations obtained by the MOST satellite were used to
characterize optical small scale variability of the young stars FU Ori and Z
CMa. Wavelet analysis for FU Ori reveals the possible existence of several 2-9
d quasi-periodic features occurring nearly simultaneously; they may be
interpreted as plasma parcels or other localized disc heterogeneities revolving
at different Keplerian radii in the accretion disc. Their periods may shorten
slowly which may be due to spiralling in of individual parcels toward the inner
disc radius, estimated at 4.8+/-0.2 R_sun. Analysis of additional multicolour
data confirms the previously obtained relation between variations in the B-V
colour index and the V magnitude. In contrast to the FU Ori results, the
oscillation spectrum of Z CMa does not reveal any periodicities with the
wavelet spectrum possibly dominated by outburst of the Herbig Be component.Comment: Accepted by MNRA
Recommended from our members
Kepler-4B: A Hot Neptune-Like Planet of A G0 Star Near Main-Sequence Turnoff
Early time-series photometry from NASA's Kepler spacecraft has revealed a planet transiting the star we term Kepler-4, at R.A. = 19(h)02(m)27.(s)68, delta = +50 degrees 08'08 '' 7. The planet has an orbital period of 3.213 days and shows transits with a relative depth of 0.87 x 10(-3) and a duration of about 3.95 hr. Radial velocity (RV) measurements from the Keck High Resolution Echelle Spectrometer show a reflex Doppler signal of 9.3(-1.9)(+1.1) m s(-1), consistent with a low-eccentricity orbit with the phase expected from the transits. Various tests show no evidence for any companion star near enough to affect the light curve or the RVs for this system. From a transit-based estimate of the host star's mean density, combined with analysis of high-resolution spectra, we infer that the host star is near turnoff from the main sequence, with estimated mass and radius of 1.223(-0.091)(+0.053) M(circle dot) and 1.487(-0.084)(+0.071) R(circle dot).We estimate the planet mass and radius to be {M(P), R(P)} = {24.5 +/- 3.8 M(circle plus), 3.99 +/- 0.21 R(circle plus)}. The planet's density is near 1.9 g cm(-3); it is thus slightly denser and more massive than Neptune, but about the same size.W. M. Keck FoundationNASA's Science Mission DirectorateAstronom
A search for transits of GJ 581\lowercase{e} and characterization of the host star variability using MOST space telescope photometry
The GJ 581 system has been amply studied since its discovery in 2005: the
number of known planets in the system has increased and their orbital
parameters are among the most precisely determined for radial velocity detected
exoplanets. We have acquired MOST space-based photometry during 2007 and 2009,
with the aims of measuring the stellar variability and searching for transits
of GJ 581e, respectively. We quantify our sensitivity to shallow transit
signals using Monte Carlo simulations, and perform a transit search within the
3 transit windows corresponding to both the circular and Keplerian
orbit ephemerides. Our analysis rules out transits for a planet with an orbital
period of 3.15 days (GJ 581 e) having a radius larger than 1.62
(or a density lower than 2.39 g cm for an orbital inclination of
90) to 2 confidence. Thus, if the planet transits, we can
exclude hydrogen, helium and water theoretical model compositions. The MOST
photometry also allows us to rule out transits of GJ 581b within the Keplerian
orbit-derived transit window for impact parameter values smaller than 0.4
and confirm previous results which exclude transits for this planet within the
circular orbit-derived transit window, for all plausible interior compositions.
We find that the stellar brightness of GJ 581 is stable to within 1%, a
characteristic which is favourable to the development of life in the habitable
zone of the system. In the 2009 photometry, we detect a stellar signal with a
period of 5.586 0.051 days, which is close to the orbital period of GJ
581b (5.37 days). However, further monitoring of the system is necessary to
verify the nature of this variation.Comment: 11 pages, 2 tables, 10 figures; accepted for publication in Ap
Stable and unstable accretion in the classical T Tauri stars IM Lup and RU Lup as observed by MOST
Results of the time variability monitoring of the two classical T Tauri
stars, RU Lup and IM Lup, are presented. Three photometric data sets were
utilised: (1) simultaneous (same field) MOST satellite observations over four
weeks in each of the years 2012 and 2013, (2) multicolour observations at the
SAAO in April - May of 2013, (3) archival V-filter ASAS data for nine seasons,
2001 - 2009. They were augmented by an analysis of high-resolution,
public-domain VLT-UT2 UVES spectra from the years 2000 to 2012. From the MOST
observations, we infer that irregular light variations of RU Lup are caused by
stochastic variability of hot spots induced by unstable accretion. In contrast,
the MOST light curves of IM Lup are fairly regular and modulated with a period
of about 7.19 - 7.58 d, which is in accord with ASAS observations showing a
well defined 7.247+/-0.026 d periodicity. We propose that this is the
rotational period of IM Lup and is due to the changing visibility of two
antipodal hot spots created near the stellar magnetic poles during the stable
process of accretion. Re-analysis of RU Lup high-resolution spectra with the
Broadening Function approach reveals signs of a large polar cold spot, which is
fairly stable over 13 years. As the star rotates, the spot-induced depression
of intensity in the Broadening Function profiles changes cyclically with period
3.71058 d, which was previously found by the spectral cross-correlation method.Comment: 14 pages, 7 figures. Accepted by MNRA
The Relational Effect Of The Rule Of Law: A Comparative Study Of Japanese And South Korean Foreign Direct Investment
Building on institutional theory, this paper examines the relationship between the relative
rule of law of home and host countries, the home country's institutional frame and foreign
direct investment (FDI). We suggest that firms based in countries with a higher level of
rule of law will invest more FDI per capita in host countries with comparable or higher
levels of legal protections. Further, companies based in countries with a lower rule of law
are accustomed to lower degrees of institutional safeguards. For these latter countries,
the comparable levels of rule of law between home and host country will not as strongly
impact FDI per capita. We test our logic through an examination of FDI from two home
countries with different levels of rule of law: Japan (high) and South Korea (medium).
Using FDI data from Japanese firms in 114 countries and South Korean firms in 118
countries, we find that while rule of law is a predictor of FDI per capita, the relative
nature of the rule of law between home and host countries in higher rule of law home
countries is also important. In addition, we discover that companies from Japan, a high
rule of law country do seek out similar or higher rule of law environments for higher
levels of FDI per capita investments while companies from a medium level rule of law
country, South Korea, are less beholden to institutional standards. Our study contributes
to the literature looking at the impact of country-level factors on foreign investment
decisions, suggesting that it is the comparative rather than absolute values that are
important to understand as well as the institutional environment in the home countr
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