274 research outputs found
Theoretical planetary mass spectra - a predition for COROT
The satellite COROT will search for close-in exo-planets around a few
thousand stars using the transit search method. The COROT mission holds the
promise of detecting numerous exo-planets. Together with radial velocity
follow-up observations, the masses of the detected planets will be known.
We have devised a method for predicting the expected planetary populations
and compared it to the already known exo-planets. Our method works by looking
at all hydrostatic envelope solutions of giant gas planets that could possibly
exist in arbitrary planetary nebulae and comparing the relative abundance of
different masses. We have completed the first such survey of hydrostatic
equilibria in an orbital range covering periods of 1 to 50 days.
Statistical analysis of the calculated envelopes suggests division into three
classes of giant planets that are distinguished by orbital separation. We term
them classes G (close-in), H, and J (large separation). Each class has distinct
properties such as a typical mass range.
Furthermore, the division between class H and J appears to mark important
changes in the formation: For close-in planets (classes G and H) the concept of
a critical core-mass is meaningless while it is important for class J. This
result needs confirmation by future dynamical analysis.Comment: 6 pages, 3 figures, MNRAS letter, accepted 2007 February
The formation of HD 149026 b
Today, many extrasolar planets have been detected. Some of them exhibit
properties quite different from the planets in our solar system and they have
eluded attempts to explain their formation. One such case is HD 149026 b. It
was discovered by Sato et al. (2005) . A transit-determined orbital inclination
results in a total mass of 114 earth masses. The unusually small radius can be
explained by a condensible element core with an inferred mass of 67 earth
masses for the best fitting theoretical model.
In the core accretion model, giant planets are assumed to form around a
growing core of condensible materials. With increasing core mass, the amount of
gravitationally bound envelope mass increases. This continues up to the
so-called critical core mass -- the largest core allowing a hydrostatic
envelope. For larger cores, the lack of static solutions forces a dynamic
evolution of the protoplanet in the process accreting large amounts of gas or
ejecting the envelope. This would prevent the formation of HD 149026 b.
By studying all possible hydrostatic equilibria we could show that HD 149026
b can remain hydrostatic up to the inferred heavy core. This is possible if it
is formed in-situ in a relatively low-pressure nebula. This formation process
is confirmed by fluid-dynamic calculations using the environmental conditions
as determined by the hydrostatic models.
We present a quantitative in-situ formation scenario for the massive core
planet HD 149026 b. Furthermore we predict a wide range of possible core masses
for close-in planets like HD 149026 b. This is different from migration where
typical critical core masses should be expected.Comment: 6 pages, 2 figures, letter MNRAS accepted 2007 Jan
Transit observations at the observatory in Grossschwabhausen: XO-1b and TrES-1
We report on observations of transit events of the transiting planets XO-1b
and TrES-1 with the AIU Jena telescope in Grossschwabhausen. Based on our IR
photometry (in March 2007) and available transit timings (SuperWASP, XO and
TLC-project-data) we improved the orbital period of XO-1b (P =
3.9414970.000006) and TrES-1 (P = 3.03007370.000006), respectively.
The new ephemeris for the both systems are presented.Comment: 4 pages, 2 figure
Giant planet formation: episodic impacts vs. gradual core growth
We describe the growth of gas giant planets in the core accretion scenario.
The core growth is not modeled as a gradual accretion of planetesimals but as
episodic impacts of large mass ratios, i.e. we study impacts of 0.02 - 1 Earth
masses onto cores of 1-15 Earth masses. Such impacts could deliver the majority
of solid matter in the giant impact regime. We focus on the thermal response of
the envelope to the energy delivery. Previous studies have shown that sudden
shut off of core accretion can dramatically speed up gas accretion. We
therefore expect that giant impacts followed by periods of very low core
accretion will result in a net increase in gas accretion rate. This study aims
at modelling such a sequence of events and to understand the reaction of the
envelope to giant impacts in more detail.
To model this scenario, we spread the impact energy deposition over a time
that is long compared to the sound crossing time, but very short compared to
the Kelvin-Helmholtz time. The simulations are done in spherical symmetry and
assume quasi-hydrostatic equilibrium.
Results confirm what could be inferred from previous studies: gas can be
accreted faster onto the core for the same net core growth speed while at the
same time rapid gas accretion can occur for smaller cores -- significantly
smaller than the usual critical core mass. Furthermore our simulations show,
that significant mass fractions of the envelope can be ejected by such an
impact
Five New Transits of the Super-Neptune HD 149026
We present new photometry of HD 149026 spanning five transits of its
"super-Neptune" planet. In combination with previous data, we improve upon the
determination of the planet-to-star radius ratio: R_p/R_star =
0.0491^{+0.0018}_{-0.0005}. We find the planetary radius to be 0.71 +/- 0.05
R_Jup, in accordance with previous theoretical models invoking a high metal
abundance for the planet. The limiting error is the uncertainty in the stellar
radius. Although we find agreement among four different ways of estimating the
stellar radius, the uncertainty remains at 7%. We also present a refined
transit ephemeris and a constraint on the orbital eccentricity and argument of
pericenter, e cos(omega) = -0.0014 +/- 0.0012, based on the measured interval
between primary and secondary transits.Comment: To appear in ApJ [19 pages
Simultaneous X-ray, radio, near-infrared, and optical monitoring of Young Stellar Objects in the Coronet cluster
Multi-wavelength (X-ray to radio) monitoring of Young Stellar Objects (YSOs)
can provide important information about physical processes at the stellar
surface, in the stellar corona, and/or in the inner circumstellar disk regions.
While coronal processes should mainly cause variations in the X-ray and radio
bands, accretion processes may be traced by time-correlated variability in the
X-ray and optical/infrared bands. Several multi-wavelength studies have been
successfully performed for field stars and approx. 1-10 Myr old T Tauri stars,
but so far no such study succeeded in detecting simultaneous X-ray to radio
variability in extremely young objects like class I and class 0 protostars.
Here we present the first simultaneous X-ray, radio, near-infrared, and optical
monitoring of YSOs, targeting the Coronet cluster in the Corona Australis
star-forming region, which harbors at least one class 0 protostar, several
class I objects, numerous T Tauri stars, and a few Herbig AeBe stars. [...]
Seven objects are detected simultaneously in the X-ray, radio, and
optical/infrared bands; they constitute our core sample. While most of these
sources exhibit clear variability in the X-ray regime and several also display
optical/infrared variability, none of them shows significant radio variability
on the timescales probed. We also do not find any case of clearly
time-correlated optical/infrared and X-ray variability. [...] The absence of
time-correlated multi-wavelength variability suggests that there is no direct
link between the X-ray and optical/infrared emission and supports the notion
that accretion is not an important source for the X-ray emission of these YSOs.
No significant radio variability was found on timescales of days.Comment: 11 pages, 11 figures, accepted for publication in A&A (06 Dec 2006
Variability of young stars: Determination of rotational periods of weak-line T Tauri stars in the Cepheus-Cassiopeia star-forming region
We report on observation and determination of rotational periods of ten
weak-line T Tauri stars in the Cepheus-Cassiopeia star-forming region.
Observations were carried out with the Cassegrain-Teleskop-Kamera (CTK) at
University Observatory Jena between 2007 June and 2008 May. The periods
obtained range between 0.49 d and 5.7 d, typical for weak-line and post T Tauri
stars.Comment: 11 pages, 26 figures, accepted to be published in A
A new dynamical modeling of the WASP-47 system with CHEOPS observations
Among the hundreds of known hot Jupiters (HJs), only five have been found to have companions on short-period orbits. Within this rare class of multiple planetary systems, the architecture of WASP-47 is unique, hosting an HJ (planet-b) with both an inner and an outer sub-Neptunian mass companion (-e and -d, respectively) as well as an additional non-transiting, long-period giant (-c). The small period ratio between planets -b and -d boosts the transit time variation (TTV) signal, making it possible to reliably measure the masses of these planets in synergy with the radial velocity (RV) technique. In this paper, we present new space- and ground-based photometric data of WASP-47b and WASP-47-d, including 11 unpublished light curves from the ESA mission CHaracterising ExOPlanet Satellite (CHEOPS). We analyzed the light curves in a homogeneous way together with all the publicly available data to carry out a global N-body dynamical modeling of the TTV and RV signals. We retrieved, among other parameters, a mass and density for planet -d of Md = 15.5 ± 0.8 Mâ and Ïd = 1.69 ± 0.22 g cmâ3, which is in good agreement with the literature and consistent with a Neptune-like composition. For the inner planet (-e), we found a mass and density of Me = 9.0 ± 0.5 Mâ and Ïe = 8.1 ± 0.5 g cmâ3, suggesting an Earth-like composition close to other ultra-hot planets at similar irradiation levels. Though this result is in agreement with previous RV plus TTV studies, it is not in agreement with the most recent RV analysis (at 2.8Ï), which yielded a lower density compatible with a pure silicate composition. This discrepancy highlights the still unresolved issue of suspected systematic offsets between RV and TTV measurements. In this paper, we also significantly improve the orbital ephemerides of all transiting planets, which will be crucial for any future follow-up
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