Datasets:

ReadingTimeMachine
/

rtm-sgt-ocr-v1

Dataset card Data Studio Files Files and versions Community

Split (1)

train · 1.53M rows

Subsets and Splits

No community queries yet

The top public SQL queries from the community will appear here once available.

source stringlengths 1 2.05k ⌀	target stringlengths 1 11.7k
In the present work we examine a slightly dilleren situation.	In the present work we examine a slightly different situation.
As in Pocllewska&Szuszkiewicz(2008) planets form a close pair and are embedded: in the gaseous disc. but this time the Super-Earth lies on the external orbit.	As in \citet{paperI} planets form a close pair and are embedded in the gaseous disc, but this time the Super-Earth lies on the external orbit.
‘This case has been already studied by Thonumes(2005) and more recently bv Pierens&Nelson(2008). (hereafter PNOS).	This case has been already studied by \citet{thommes05} and more recently by \citet{pierens} (hereafter PN08).
ποιος(2005) has found that a Jupiter mass planet can act. at least for à certain time. as a safety net Lor low-mass planets. capturing them into orbital commoensurabilities.	\citet{thommes05} has found that a Jupiter mass planet can act, at least for a certain time, as a safety net for low-mass planets, capturing them into orbital commensurabilities.
In his calculations. the low-mass planet. which is allowed. to accrete the mass. migrates towards the Jupiter and ends up in à 1:2 or 2:3 resonance depending on the surface density of the disc.	In his calculations, the low-mass planet, which is allowed to accrete the mass, migrates towards the Jupiter and ends up in a 1:2 or 2:3 resonance depending on the surface density of the disc.
Contrary to his result. PNOS have noticed that a low-mass planet (in the range of 3.5 - 20 AL, ) can be trapped at the outer edge of the gap opened by the gas giant.	Contrary to his result, PN08 have noticed that a low-mass planet (in the range of 3.5 - 20 $M_{\oplus}$ ) can be trapped at the outer edge of the gap opened by the gas giant.
Planets cannot therefore get close enough as it is necessary to attain a mean motion resonance.	Planets cannot therefore get close enough as it is necessary to attain a mean motion resonance.
Such planet trapping mechanism is possible at the steep and. positive surface density. gradient in the radial profile of the gaseous disc where. the corotation orque compensates the dillerential Lindblad torque (Massetetal.2006).	Such planet trapping mechanism is possible at the steep and positive surface density gradient in the radial profile of the gaseous disc where, the corotation torque compensates the differential Lindblad torque \citep{masset}.
. Alore recently Paardekooper&Papaloizou(2000) have studied the nonlinear cllects arising in the coorbital region of planets of a few Earth masses.	More recently \citet{paandpa} have studied the nonlinear effects arising in the coorbital region of planets of a few Earth masses.
They have ound that any. positive density gradient in the disc can act as à protoplanctary trap.	They have found that any positive density gradient in the disc can act as a protoplanetary trap.
The investigations of Thonunes(2005) have been xrformed. using a hivbrid. code. that combines an N-bocly component with a one-dimensional viscous disc model.	The investigations of \citet{thommes05} have been performed using a hybrid code, that combines an N-body component with a one-dimensional viscous disc model.
In his way the effects of Lindblad torques are well reproduced. »it the corotation torques acting on the low-mass planet are not taken into account.	In this way the effects of Lindblad torques are well reproduced, but the corotation torques acting on the low-mass planet are not taken into account.
Emploving a 2D. hvedrodynamical code. PNOS have been able to include properly both types of torques.	Employing a 2D hydrodynamical code, PN08 have been able to include properly both types of torques.
Lt has been shown by PNOS that the initially convergent migration of a Jupiter mass gas giant and an outer planet [ess massive than 20 M, stops when the Iow-mass planet approaches the outer edge of the gap formed bv the gas giant.	It has been shown by PN08 that the initially convergent migration of a Jupiter mass gas giant and an outer planet less massive than 20 $M_{\oplus}$ stops when the low-mass planet approaches the outer edge of the gap formed by the gas giant.
Later on. the low-mass planets migrate outward.	Later on, the low-mass planets migrate outward.
In the present work we confirm the results of PNOS in the case of a Super-Earth and a Jupiter-like planet.	In the present work we confirm the results of PN08 in the case of a Super-Earth and a Jupiter-like planet.
The only cülference is that in the calculations of PNOS the low-mass planet was able to acercte matter from the clise and if its mass exceeded the value of 20 AL). the planets ended up in à mean-motion resonance.	The only difference is that in the calculations of PN08 the low-mass planet was able to accrete matter from the disc and if its mass exceeded the value of 20 $M_\oplus$, the planets ended up in a mean-motion resonance.
In this paper we are interested in Super-Earths. so we did not take into account aceretion.	In this paper we are interested in Super-Earths, so we did not take into account accretion.
As an extension. of the work of PNOS. we have investigated. the evolution of a Super-Earth also in the presence of Sub-Jupiter eas giants. whose masses are lower than that of Jupiter.	As an extension of the work of PN08, we have investigated the evolution of a Super-Earth also in the presence of Sub-Jupiter gas giants, whose masses are lower than that of Jupiter.
For typical disc properties the gap opened by the gas giant. is very wide and the positions of all first order mean motion commoensurabilities are located inside the region allected by the gap.	For typical disc properties the gap opened by the gas giant is very wide and the positions of all first order mean motion commensurabilities are located inside the region affected by the gap.
LE the eas giant. is assumed to be less massive than Jupiter (e.g. 0.5427). the gap opened by the planet is narrower. which gives a chance for attaining a first order mean motion resonance.	If the gas giant is assumed to be less massive than Jupiter (e.g. $0.5 M_J$ ), the gap opened by the planet is narrower, which gives a chance for attaining a first order mean motion resonance.
However. in this situation the migration of the eas giant is faster than that of the low-mass planet causing the divergent relative motion of both planets.	However, in this situation the migration of the gas giant is faster than that of the low-mass planet causing the divergent relative motion of both planets.
For this reason. in order to ect the commensurabilitv one needs to slow down the Sub-Jupiter or to speed up the Super-Earth.	For this reason, in order to get the commensurability one needs to slow down the Sub-Jupiter or to speed up the Super-Earth.
Finally. we have achieved the 1:2 mean motion resonance for very thin clises and low surface density.	Finally, we have achieved the 1:2 mean motion resonance for very thin discs and low surface density.
This configuration. however. has not been maintained till the end of the simulations.	This configuration, however, has not been maintained till the end of the simulations.
This paper is organized as follows.	This paper is organized as follows.
In. Section 2 we describe our. numerical set-up.	In Section 2 we describe our numerical set-up.
In. Section. 3 we present the procedure. used. in order to achieve the convergent migration ofa Super-ISarth and a Jupiter-like planet.	In Section 3 we present the procedure used in order to achieve the convergent migration of a Super-Earth and a Jupiter-like planet.
Section 4 ds dedicated. to the results obtained in the evolution of such a system of planets.	Section 4 is dedicated to the results obtained in the evolution of such a system of planets.
We also discuss in this Section the eccentricity behaviour together with the analysis of the sensitivity of our results to numerical parameters. and	We also discuss in this Section the eccentricity behaviour together with the analysis of the sensitivity of our results to numerical parameters and
events. bad pixels. and events registered too close to chip gaps by requiring "FLAGZO" and "PATTERN < 4.	events, bad pixels, and events registered too close to chip gaps by requiring “FLAG=0” and “PATTERN $\leq$ 4”.
Inspection of lightcurves made from the data revealed no evidence of background flaring. and the entire 42 ksee was used to generate EPIC-pn spectra.	Inspection of lightcurves made from the data revealed no evidence of background flaring, and the entire 42 ksec was used to generate EPIC-pn spectra.
Source and background spectra were made in the standard way by grouping PI channels 0-20479 by a factor of 5.	Source and background spectra were made in the standard way by grouping PI channels 0–20479 by a factor of 5.
The source spectrum was extracted between 20-56 in RAWX. and using the full RAWY range.	The source spectrum was extracted between 20–56 in RAWX, and using the full RAWY range.
Àn adjacent background region was extracted. and the spectra were properly normalized.	An adjacent background region was extracted, and the spectra were properly normalized.
Custom redistribution matrix files (rmfs) and ancillary response files (arfs) for the spectra made using the SAS tasks "rmfgen" and "arfgzen".	Custom redistribution matrix files (rmfs) and ancillary response files (arfs) for the spectra made using the SAS tasks “rmfgen” and “arfgen”.
We also made MOS-1 and MOS-2 event lists and spectra.	We also made MOS-1 and MOS-2 event lists and spectra.
The MOS-I camera was operated in "timing" mode. which is seldom used.	The MOS-1 camera was operated in “timing” mode, which is seldom used.
The MOS-2 camera was operated in "full-frame" mode. and therefore suffered photon pile-up.	The MOS-2 camera was operated in “full-frame” mode, and therefore suffered photon pile-up.
While results from both MOS cameras confirm the pn results we report below. we regard them as less reliable and do not consider them in this work.	While results from both MOS cameras confirm the pn results we report below, we regard them as less reliable and do not consider them in this work.