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The [Fe u] profile is. on the other hand. marginally resolved. | The [Fe ] profile is, on the other hand, marginally resolved. |
In the echelle data of and Takamietal.(2005) a radial velocity of 140. wwith respect to the svstemic velocity. was assigned to (his component. | In the echelle data of \citet{dav03} and \citet{tak05} a radial velocity of $\sim 140$ with respect to the systemic velocity was assigned to this component. |
Prestunably (his compact. hieh-velocity. emission derives [rom a discrete knot or shock front near the base of the jet. rather than from an extended emission region. | Presumably this compact, high-velocity emission derives from a discrete knot or shock front near the base of the jet, rather than from an extended emission region. |
In the II» data. we see an interesting trend where the size (FWIIM) of each component increases with distance from the source (Table 1)). | In the $_2$ data, we see an interesting trend where the size (FWHM) of each component increases with distance from the source (Table \ref{table1}) ). |
Moreover. if the H» and [Fe u] trace the same jet material. this trend. extends to the[Fe 11] data: the closer a component is to the | Moreover, if the $_2$ and [Fe ] trace the same jet material, this trend extends to the[Fe ] data; the closer a component is to the |
The angular power spectrum of the cosmic microwave background (CMB) has much to teach us about the nature of the Universe in which we live ((Hu. Sugiyama. Silk 1997). | The angular power spectrum of the cosmic microwave background (CMB) has much to teach us about the nature of the Universe in which we live \markcite{hu97b}( (Hu, Sugiyama, Silk 1997). |
Measurements are improving rapidly ((de 2000: 2000; 2001). and for a wide variety of theoretical scenarios the predicted spectra can be calculated accurately (Zaldarriaga 2000). | Measurements are improving rapidly \markcite{debernardis00,hanany00,padin01}( 2000; 2000; 2001), and for a wide variety of theoretical scenarios the predicted spectra can be calculated accurately \markcite{zaldarriaga00}( 2000). |
Comparison of the data and models allows quantitative constraints to be placed on the parameters of the Universe in which we find ourselves. and is the subject of this paper. | Comparison of the data and models allows quantitative constraints to be placed on the parameters of the Universe in which we find ourselves, and is the subject of this paper. |
The Degree Angular Scale Interferometer (DASI)). along with its sisterinstrument the CBI ((Padin 2001) and the VSA (Jones 1996). Is one of several new compact interferometers specifically designed for observations of the CMB. | The Degree Angular Scale Interferometer ), along with its sisterinstrument the CBI \markcite{padin01}( 2001) and the VSA \markcite{jones96}( 1996), is one of several new compact interferometers specifically designed for observations of the CMB. |
This paper ts the third in a set of three. | This paper is the third in a set of three. |
Paper I ((Leitch 2001) gives a detailed description of the instrument. observations. and data calibration. | Paper I \markcite{leitch01}( (Leitch 2001) gives a detailed description of the instrument, observations, and data calibration. |
Paper II ((Halverson 2001) focuses on the extraction of the angular power spectrum from the calibrated interferometric data. and provides band-power estimates of the angular power spectrum of the CMB. | Paper II \markcite{halverson01}( (Halverson 2001) focuses on the extraction of the angular power spectrum from the calibrated interferometric data, and provides band-power estimates of the angular power spectrum of the CMB. |
In this paperwe combine the low-/ measurements made by the COBE-DMR instrument ((Bennett 1996) with the new measurements from tto constrain the parameters of cosmological models. | In this paperwe combine the $l$ measurements made by the COBE-DMR instrument \markcite{bennett96}( 1996) with the new measurements from to constrain the parameters of cosmological models. |
The layout of this paper is as follows. | The layout of this paper is as follows. |
The considerations which drive our selection of the model and parameter space to probe are detailed in refsec:grid.. | The considerations which drive our selection of the model and parameter space to probe are detailed in \\ref{sec:grid}. |
In refsec:datacomp we review the method used to compare band power data to theoretical spectra. | In \\ref{sec:datacomp} we review the method used to compare band power data to theoretical spectra. |
The results of this comparison are described in refsec:res.. and in we draw some conclusions. | The results of this comparison are described in \\ref{sec:res}, and in we draw some conclusions. |
Following the discovery of the CMB. and the realization that the Universe went through a hot plasma epoch. it was proposed that adiabatic density perturbations in that plasma would lead to acoustic oscillations ((Peebles 1970). and a series of harmonic peaks in the angular power spectrum ((Doroshkevich.Zeldovich. 1978). | Following the discovery of the CMB, and the realization that the Universe went through a hot plasma epoch, it was proposed that adiabatic density perturbations in that plasma would lead to acoustic oscillations \markcite{peebles70}( 1970), and a series of harmonic peaks in the angular power spectrum \markcite{doroshkevich78}(, 1978). |
It was assumed that the initial fluctuations were scale invariant only because this is the simplest possible case. | It was assumed that the initial fluctuations were scale invariant only because this is the simplest possible case. |
It was notuntil later that (New) Inflation was proposed ((Guth 1982;Bardeen.Steinhardt. 1983: 1982: Starobinsky 1982) — an elegant cosmo-genic mechanism which naturally produces such conditions. | It was notuntil later that (New) Inflation was proposed \markcite{guth82,bardeen83,hawking82,starobinskii82}( 1982;, 1983; 1982; Starobinsky 1982) — an elegant cosmo-genic mechanism which naturally produces such conditions. |
The simplest versions of this theory also make the firm prediction that the Universe is exactly flat. 1.e.. has zero net spatial curvature. | The simplest versions of this theory also make the firm prediction that the Universe is exactly flat, i.e., has zero net spatial curvature. |
Although Inflation sets the stage at the beginning of the plasma epoch it has nothing to say about the contents of the Universe. | Although Inflation sets the stage at the beginning of the plasma epoch it has nothing to say about the contents of the Universe. |
Over the last several decades a wealth of evidence has accumulated for the existence of some form of gravitating matter which does not interact with ordinary baryonic material: the so-called cold dark matter (CDM). | Over the last several decades a wealth of evidence has accumulated for the existence of some form of gravitating matter which does not interact with ordinary baryonic material; the so-called cold dark matter (CDM). |
Conflicting theoretical expectations and experimental measurements led to the proposal that a third component is present — an intrinsic vacuum energy. | Conflicting theoretical expectations and experimental measurements led to the proposal that a third component is present — an intrinsic vacuum energy. |
This three component model is the scenario we have chosen to consider. | This three component model is the scenario we have chosen to consider. |
The density required to produce zero net spatial curvature is referred to as the critical density p,=3H5/(8xG). where Hy is the Hubble constant (Hp=1005 km s! Mpe!). | The density required to produce zero net spatial curvature is referred to as the critical density $\rho_c=3H_0^2/(8\pi G)$, where $H_0$ is the Hubble constant $H_0 \equiv 100 h$ km $^{-1}$ $^{-1}$ ). |
It is convenient to measure the present day density of à component of the Universe in units of p.. denoting this €;: the density of baryonic matter Q,.. the density of CDM O,,,.. and the | It is convenient to measure the present day density of a component of the Universe in units of $\rho_c$ , denoting this $\Omega_i$ : the density of baryonic matter , the density of CDM , and the |
within externa ealaxics and hence the identification. of any line variaημίν as being due to microlensing may be problematic. | within external galaxies and hence the identification of any line variability as being due to microlensing may be problematic. |
While this paper has demonstrated: that microlensing induced. absorption line variability is not perferetiy correated with the variability of the brightness of the macrolensecl images. some correlation does exist. | While this paper has demonstrated that microlensing induced absorption line variability is not perferctly correlated with the variability of the brightness of the macrolensed images, some correlation does exist. |
Hence. long term. photo-spectral monitoring at high resolution of potential systems. such as1830-211.. is required before such a conclusiin is confirmed. | Hence, long term photo-spectral monitoring at high resolution of potential systems, such as, is required before such a conclusion is confirmed. |
GEL. gratefully| acknowledges discussions with Joachim Wonmbsgansse and Rachel Webster on aspects of microlensing. | GFL gratefully acknowledges discussions with Joachim Wambsganss and Rachel Webster on aspects of microlensing. |
Joachim Wanmbseanss is also thanked for providing his code on which this study is based. | Joachim Wambsganss is also thanked for providing his code on which this study is based. |
We als» thank “Terry Bridges for allowing us to hammer oclin. the computer on which these simulations were undertaken. | We also thank Terry Bridges for allowing us to hammer odin, the computer on which these simulations were undertaken. |
Phe referee. Stuart νο, is thanked for comment which improved this contribution. | The referee, Stuart Wyithe, is thanked for comment which improved this contribution. |
Although the number of pulsars discovered. recently in modern search campaigns increased. enormouslv. the observed: pulsar. population is still a small fraction of the neutron star population in the Galaxy. | Although the number of pulsars discovered recently in modern search campaigns increased enormously, the observed pulsar population is still a small fraction of the neutron star population in the Galaxy. |
Most. of them will never be detected as radio pulsars due to misalignment of their beams with our lineofsight (Iοs). | Most of them will never be detected as radio pulsars due to misalignment of their beams with our line–of–sight (l–o–s). |
However. many of those whose beams point towards the Earth. still await detection in future. more sensitive pulsar surveys. | However, many of those whose beams point towards the Earth still await detection in future, more sensitive pulsar surveys. |
Pherefore. a more or less complete knowledge about Galactic pulsar population can be obtained. only by means of. statistical considerations. | Therefore, a more or less complete knowledge about Galactic pulsar population can be obtained only by means of statistical considerations. |
Statistical studies of the pulsewidth in mean profiles of radio pulsars is an important tool for investigations of the geometry of pulsar. radiation. | Statistical studies of the pulse–width in mean profiles of radio pulsars is an important tool for investigations of the geometry of pulsar radiation. |
One especially important. parameter that can be derived. from such studies is the inclination angle between the magnetic and the spin pulsar axes. | One especially important parameter that can be derived from such studies is the inclination angle between the magnetic and the spin pulsar axes. |
Early studies were carried. out bv Henry&Paik (1960).. Roberts&Sturrock(1972. 1973).. Backer(1976) ancl Manchester Lyne (1977. hereafter. ML77)). | Early studies were carried out by \citet{hp69}, , \citet{rs72, rs73}, \citet{b76} and Manchester Lyne (1977, hereafter \citet{ml77}) ). |
Since the amount of the available cata was small. these papers sullered from. problems of small number statistics. | Since the amount of the available data was small, these papers suffered from problems of small number statistics. |
A more complete work was performed bv Proszviski(1979) and Lyne&Alanehester(1955). who analyzed samples of about 200. pulsewidth data measurecl near 400 MlIz. | A more complete work was performed by \citet{p79} and \citet{lm88}, who analyzed samples of about 200 pulse–width data measured near 400 MHz. |
Although the database usecin | Although the database usedin |
gravity, a gap has been created in the m—1 Alfvénn continuum. | gravity, a gap has been created in the $m=1$ Alfvénn continuum. |
However, m=0 and m=2 slow continua of the coupling scheme slightly mismatch the PHOENIX results. | However, $m=0$ and $m=2$ slow continua of the coupling scheme slightly mismatch the PHOENIX results. |
This mismatch is because by our neglect of the coupling with m=—1 and m=3 slow continua. | This mismatch is because by our neglect of the coupling with $m=-1$ and $m=3$ slow continua. |
In the plot, these continua are represented by the crosses with non-zero frequency in combination without a solid line. | In the plot, these continua are represented by the crosses with non-zero frequency in combination without a solid line. |
At four different radial flux coordinates, s+0.82, sez0.837, s:0.973, and s©0.978 a Amm1 gap was produced (note the color change of the solid lines about these radii). | At four different radial flux coordinates, $s \approx 0.82$, $s \approx 0.837$, $s \approx 0.973$, and $s\approx 0.978$ a $\Delta m=1$ gap was produced (note the color change of the solid lines about these radii). |
As expected, the four-mode coupling scheme only partly captures this kind of coupling. | As expected, the four-mode coupling scheme only partly captures this kind of coupling. |
Therefore, about these Am=1 gaps there is a mismatch between the results of both methods, and a separate detailed analysis of the Am=1 coupling schemes appears to be required. | Therefore, about these $\Delta m=1$ gaps there is a mismatch between the results of both methods, and a separate detailed analysis of the $\Delta m=1$ coupling schemes appears to be required. |
The last equilibrium of this subsection that we discuss is the one with strong gravity g—1.000. | The last equilibrium of this subsection that we discuss is the one with strong gravity $g=1.000$. |
The temperature is assumed to be a flux function. | The temperature is assumed to be a flux function. |
For this equilibrium, one observes the onset of the double layered structure in the pressure and density as demonstrated in our accompanying paper (7). | For this equilibrium, one observes the onset of the double layered structure in the pressure and density as demonstrated in our accompanying paper \citep{Blokland_2011A}. . |
The results for the m—1 Alfvénn and slow continuum show excellent agreement near the q=1 surface (se 0.927). | The results for the $m=1$ Alfvénn and slow continuum show excellent agreement near the $q=1$ surface $s \approx 0.927$ ). |
Owing to the stronger gravity compared to the previous case, the gap in m—1 Alfvénn continuum is larger. | Owing to the stronger gravity compared to the previous case, the gap in $m=1$ Alfvénn continuum is larger. |
Near this surface, the previously mentioned mismatchof both the m=0 | Near this surface, the previously mentioned mismatchof both the $m=0$ |
tecently a subset of exoplanets orbiting extremely. close to heir host stars with periods less than 1 cay have been discovered. | Recently a subset of exoplanets orbiting extremely close to their host stars with periods less than 1 day have been discovered. |
Prime examples of these are the planets WASD-18b. which was discovered to be orbiting a 1.24M.. starevery 94 clavs (2): WASP-19b (orbital period = 0.79 days: 2): and C'orot-Tb (orbital period = 0.85 days: ?)). | Prime examples of these are the planets WASP-18b, which was discovered to be orbiting a $M_{\odot}$ starevery 0.94 days \citealt{hellier09}) ); WASP-19b (orbital period = 0.79 days; \citealt{hebb10}) ); and Corot-7b (orbital period = 0.85 days; \citealt{leger09}) ). |
These planets are subject to [arge tidal forces and can be used as tests of ical clissipation theory. | These planets are subject to large tidal forces and can be used as tests of tidal dissipation theory. |
In this scenario. the close proximity of the exoplanet to the host. star raises a tidal bulge on 1e stellar surface. | In this scenario, the close proximity of the exoplanet to the host star raises a tidal bulge on the stellar surface. |
This in turn exerts an additional torque which drains angular momentum from the planetary. orbit Or systems where the orbital period. is shorter than the stellar rotation period. | This in turn exerts an additional torque which drains angular momentum from the planetary orbit for systems where the orbital period is shorter than the stellar rotation period. |
In the case of WASP-I8. the tidal dissipation is such jt assuming a tidal quality factor Z2. (this is normally denoted Q but we have changed this to distinguish it from 1e quacdrupole moment used earlier) found from studies of rinaries and the giant. planets in our Solar System. means iu the planet would. be tidallv disrupted. in 1 Myr. | In the case of WASP-18, the tidal dissipation is such that assuming a tidal quality factor $D$ (this is normally denoted $Q$ but we have changed this to distinguish it from the quadrupole moment used earlier) found from studies of binaries and the giant planets in our Solar System means that the planet would be tidally disrupted in $\sim$ 1 Myr. |
Since the system's age is ~5 Cyr. 7. conclude that either rev have caught WASDP-ISb in an extremely rare state. or iu DD ds much higher than expected. | Since the system's age is $\sim$ 5 Gyr, \cite{hellier09}
conclude that either they have caught WASP-18b in an extremely rare state, or that $D$ is much higher than expected. |
2 quote a perio change of -0.000%3 (10°¢D) s !. | \cite{hellier09}
quote a period change of -0.00073 $^6$ /D) s $^{-1}$. |
For our solar svstem. D=WwW10" leading to orbital period. changes of 28 s alter 10 vr for D=10°. | For our solar system, $D = 10^5 - 10^6$ leading to orbital period changes of 28 s after 10 yr for $D = 10^6$. |
Therefore. transit timing studies of WASD-ISb are vitally important since the tidal decay shoul be directly measurable in this svstem. | Therefore, transit timing studies of WASP-18b are vitally important since the tidal decay should be directly measurable in this system. |
This would allow our understanding of tidal dissipation to be tested. and. woul also allow the stellar interior to be probed since the value of D depends on how waves generated by tides are dissipated. | This would allow our understanding of tidal dissipation to be tested and would also allow the stellar interior to be probed since the value of $D$ depends on how waves generated by tides are dissipated. |
The magnitude of the Applegate effect we have estimated for WASP-IS leads to ο variations of the order of 10's of seconds on decade timescales approximately the same as predicted due to tidal decay. | The magnitude of the Applegate effect we have estimated for WASP-18 leads to O–C variations of the order of 10's of seconds on decade timescales – approximately the same as predicted due to tidal decay. |
Such variations could easily. either mask. or mimic (briellv). or even temporarily any. period change caused by tidal decay. especially if the tidal quality factor is higher than 107. | Such variations could easily either mask, or mimic (briefly), or even temporarily any period change caused by tidal decay, especially if the tidal quality factor is higher than $^6$. |
Vhus. for WASP-ISb. caution has to be exercised in interpreting the nature of any detected. transit-time variations. since these will consist of a quasi-periodic variation on the timescale of the stellar activity evele superimposed on a steady trend of decreasing period. due to orbital decay. | Thus, for WASP-18b, caution has to be exercised in interpreting the nature of any detected transit-time variations, since these will consist of a quasi-periodic variation on the timescale of the stellar activity cycle super-imposed on a steady trend of decreasing period due to orbital decay. |
Only by observing over the course of an activity evele could. one begin. to reliably distinguish between the two mechanisms. | Only by observing over the course of an activity cycle could one begin to reliably distinguish between the two mechanisms. |
Thus. WASP-I8 is unlikely to reveal its tidal dissipation history (or future) for several vears vet. | Thus, WASP-18 is unlikely to reveal its tidal dissipation history (or future) for several years yet. |
Finally, we discuss the use of accurate transit timing as a means to probe the nature of the magnetic field generating dvnamo operating in the host stars’ interior. | Finally, we discuss the use of accurate transit timing as a means to probe the nature of the magnetic field generating dynamo operating in the host stars' interior. |
The study of the Applegate mechanism via eclipse timings of eclipsing binaries is often confused. with orbital period variations caused by angular momentum losses or exchanges. | The study of the Applegate mechanism via eclipse timings of eclipsing binaries is often confused with orbital period variations caused by angular momentum losses or exchanges. |
These include elfects due to magnetic braking ancl mass transfer. | These include effects due to magnetic braking and mass transfer. |
We propose that transiting cxoplanct svstems. by comparison. provide much cleaner laboratories in which to study such cllects. | We propose that transiting exoplanet systems, by comparison, provide much cleaner laboratories in which to study such effects. |
Furthermore. unlike in the ticlally locked: binary systems. exoplanet svstems have the crucial ingredient of a dilference between the stellar rotation perioc and its orbital period (the orbital period of the exoplanet). | Furthermore, unlike in the tidally locked binary systems, exoplanet systems have the crucial ingredient of a difference between the stellar rotation period and its orbital period (the orbital period of the exoplanet). |
If variations are seen at a level that correlates with the predictions of “Table 1. for two stars with similar orbita periods but cifferent rotation periods. then this woutle provide good evidence that the Applegate mechanism. is at work. | If variations are seen at a level that correlates with the predictions of Table \ref{tab:trans} for two stars with similar orbital periods but different rotation periods, then this would provide good evidence that the Applegate mechanism is at work. |
Naturally. however. one. should be aware tha gravitational perturbations caused. by an additional lone-period planet. in. the system could. initially be confuse with variations due to the Applegate mechanism. | Naturally, however, one should be aware that gravitational perturbations caused by an additional long-period planet in the system could initially be confused with variations due to the Applegate mechanism. |
Thus. the quasi-periodic nature of such variations has to be firmly established before one can be confident that such T'EVs can be used to probe the stellar ἂνπαιο. | Thus, the quasi-periodic nature of such variations has to be firmly established before one can be confident that such TTVs can be used to probe the stellar dynamo. |
7T showed that cilfercnt civnamo mechanisms result in different observable manifestations of the Applegate cllect. | \cite{lanza98} showed that different dynamo mechanisms result in different observable manifestations of the Applegate effect. |
If an a ἄνπαπιο is in operation then the quasi-evclic orbital period. modulations should occur on the same timescale as the spot coverage modulation (ee. over Ll vears in the case of our Sun). | If an $\alpha \Omega$ dynamo is in operation then the quasi-cyclic orbital period modulations should occur on the same timescale as the spot coverage modulation (e.g. over 11 years in the case of our Sun). |
In contrast. if an a7Q dynamo operates then the observed orbital period mocdulation should occur over a timescale twice as long as the period of the spot modulation ( 22 vears in the case of our Sun). | In contrast, if an $\alpha^2 \Omega$ dynamo operates then the observed orbital period modulation should occur over a timescale twice as long as the period of the spot modulation $\sim$ 22 years in the case of our Sun). |
Given the large number of transiting exoplanet systems with host stars (with widelv varving fundamental parameters such às age. rotation rate. masses etc.) | Given the large number of transiting exoplanet systems with host stars (with widely varying fundamental parameters such as age, rotation rate, masses etc.) |
that will be discovered by space-missions such as Ixepler ancl Plato. long-term svstematic monitoring for VEVs may reveal the nature of the dynamo mechanism at work. | that will be discovered by space-missions such as Kepler and Plato, long-term systematic monitoring for TTVs may reveal the nature of the dynamo mechanism at work. |
We have estimated the likely transit. timing variations induced hy changes in the quadrupole moment of the host star in transiting exoplanet svstems driven by the Applegate ellect. | We have estimated the likely transit timing variations induced by changes in the quadrupole moment of the host star in transiting exoplanet systems driven by the Applegate effect. |
Depending on the length of the activity evcle. PPVs of several minutes are plausible for a number of the currently known transiting exoplanets. | Depending on the length of the activity cycle, TTVs of several minutes are plausible for a number of the currently known transiting exoplanets. |
While the timescales and sizes of Applegate driven T'EVs are of the wrong magnitude to be confused. with PPYs driven by additional. planets. in mean motion resonances. there appears to be much scope for confusion with T'PVs caused by light travel time elfects caused by massive. Jupiter-like planets on wide orbits. | While the timescales and sizes of Applegate driven TTVs are of the wrong magnitude to be confused with TTVs driven by additional planets in mean motion resonances, there appears to be much scope for confusion with TTVs caused by light travel time effects caused by massive, Jupiter-like planets on wide orbits. |
The magnitude of T'PVs riven bv the Applegate mechanism also grow as the star-planet separation decreases (assuming all other factors are equal). | The magnitude of TTVs driven by the Applegate mechanism also grow as the star-planet separation decreases (assuming all other factors are equal). |
Indeed. for. the shortest. period. transiting exoplanets. such as WASP-Isb. the Applegate mechanism could. potentially be mistaken for orbital period. changes due to tidal dissipation. | Indeed, for the shortest period transiting exoplanets, such as WASP-18b, the Applegate mechanism could potentially be mistaken for orbital period changes due to tidal dissipation. |
Indeed. the orbital decay. due to tical dissipation could. even be temporarily reversed since the orbital period variations due to the Applegate elfect can take on either sign. | Indeed, the orbital decay due to tidal dissipation could even be temporarily reversed since the orbital period variations due to the Applegate effect can take on either sign. |
We therefore urge caution when interpreting PPVs. especially those that appear to be occurring on timescales of vears to decades. | We therefore urge caution when interpreting TTVs, especially those that appear to be occurring on timescales of years to decades. |
In all cases. the clear signature that the Applegate effect is at work is that the TEVs are quasi-periodic. | In all cases, the clear signature that the Applegate effect is at work is that the TTVs are quasi-periodic. |
Only once the strict. periodicity of any “PPV has been ascertained. should investigators be confident in their final interpretation. | Only once the strict periodicity of any TTV has been ascertained should investigators be confident in their final interpretation. |
Finally. an alternative mechanism for driving quasi- stellar quadrupole. variations (and. hence. orbital period variations) was put forward by 2.. | Finally, an alternative mechanism for driving quasi-periodic stellar quadrupole variations (and hence orbital period variations) was put forward by \cite{lanza98}. . |
This rests on the principle that changes in the azimuthal magnetic field | This rests on the principle that changes in the azimuthal magnetic field |
among the planetary systems with the shortest orbital periods and should. therefore. be susceptible to these effects. | among the planetary systems with the shortest orbital periods and should, therefore, be susceptible to these effects. |
A gravitationally bound stellar companion influences. the dynamies of the ssystem. | A gravitationally bound stellar companion influences the dynamics of the system. |
In particular. it slightly disturbs the planetary orbit. | In particular, it slightly disturbs the planetary orbit. |
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