Kinematics of coronal rain in a transversely oscillating loop: Ponderomotive force and rainexcited oscillations
^{1} Department of Physics, University of Warwick, Coventry CV4 7AL, UK
email: Erwin.Verwichte@warwick.ac.uk
^{2} School of Mathematics and Statistics, University of St. Andrews, St Andrews KY16 9SS, UK
Received: 1 September 2016
Accepted: 2 November 2016
Context. Coronal rain is composed of cool dense blobs that form in solar coronal loops and are a manifestation of catastrophic cooling linked to thermal instability. Once formed, rain falls towards the solar surface at subballistic speeds, which is not well understood. Pressure forces seem to be the prime candidate to explain this. In many observations rain is accompanied by transverse oscillations and the interaction between rain and these oscillations needs to be explored.
Aims. Therefore, an alternative kinematic model for coronal rain kinematics in transversely oscillating loops is developed to understand the physical nature of the observed subballistic falling motion of rain. This model explicitly explores the role of the ponderomotive force arising from the transverse oscillation on the rain motion and the capacity of rain to excite wave motion.
Methods. An analytical model is presented that describes a rain blob guided by the coronal magnetic field supporting a onedimensional shear Alfvén wave as a point mass on an oscillating string. The model includes gravity and the ponderomotive force from the oscillation acting on the mass and the inertia of the mass acting on the oscillation.
Results. The kinematics of rain in the limit of negligible rain mass are explored and falling and trapped regimes are found, depending on wave amplitude. In the trapped regime for the fundamental mode, the rain blob bounces back and forth around the loop top at a long period that is inversely proportional to the oscillation amplitude. The model is compared with several observational rain studies, including one indepth comparison with an observation that shows rain with upanddown bobbing motion. The role of rain inertia in exciting transverse oscillations is explored in inclined loops.
Conclusions. It is found that the model requires displacement amplitudes of the transverse oscillation that are typically an order of magnitude larger than observed to explain the measured subballistic motion of the rain. Therefore, it is concluded that the ponderomotive force is not the primary reason for understanding subballistic motion, but it plays a role in cases of large loop oscillations. The appearance of rain causes the excitation of smallamplitude transverse oscillations that may explain observed events and provide a seismological tool to measure rain mass.
Key words: Sun: corona / Sun: oscillations / Sun: activity / magnetohydrodynamics (MHD) / methods: analytical / waves
© ESO, 2017
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (http://creativecommons.org/licenses/by/4.0),
which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
1. Introduction
Coronal rain are cool dense blobs that form in warm active region loops and fall along the guiding magnetic field to the solar surface (Kawaguchi 1970; Leroy 1972; Athay et al. 1980; Schrijver 2001; De Groof et al. 2004; de Groof et al. 2005; Vashalomidze et al. 2015). They are traditionally observed in chromospheric lines, such as Hα or Ca II H, as well as in transition region lines. But they can also be detected in absorption in the extreme ultraviolet (EUV). It is believed that coronal rain is a manifestation of catastrophic cooling of coronal loop plasma in response to localised heating near the loop footpoints (e.g. Müller et al. 2005; Klimchuk et al. 2008; Antolin et al. 2010). As such it is an important characteristic of the coronal heating process.
Using the Solar Optical Telescope (SOT) on board the Hinode satellite (Tsuneta et al. 2008) and the CRisp Imaging SpectroPolarimeter at the Swedish 1 m Solar Telescope (Scharmer et al. 2003, 2008), Antolin et al. (2010), Antolin & Rouppe van der Voort (2012), Antolin et al. (2015) showed, with ondisk and limb observations, that coronal rain is a common occurrence in warm active region loops. Coronal rain is dynamic with lifetimes of a few minutes, widths of several hundred km and lengths of a few Mm. The blobs become more thinner and elongated towards the footpoints. Their small sizes makes them particularly useful for probing the local magnetic field structure (Antolin & Rouppe van der Voort 2012). Coronal rain has been measured with temperatures ranging between 3000 K to 150 000 K (Levine & Withbroe 1977; Müller et al. 2005) and is expected from simulations to have a density of 10^{16}–10^{18} m^{3} (Antolin et al. 2010; Luna et al. 2012; Fang et al. 2013, 2015); this value is confirmed by observations (Antolin et al. 2015). The downflow speed of the rain ranges between 30 up to supersonic speeds of 200 km s^{1} with an average of 60−70 km s^{1} (Ahn et al. 2014; Kleint et al. 2014; Antolin et al. 2015; Straus et al. 2015).
The downwards acceleration is usually of the order of 80 ± 30 m s^{2} (Antolin & Rouppe van der Voort 2012), which is substantially subballistic, even when taking the loop geometry and line of sight into account. This would mean that other forces act upwards along the loop against gravity. The prime candidate force arises from the coronal plasma below the rain blob that is being compressed as the rain falls towards the surface (Müller et al. 2003; Oliver et al. 2014). The resulting drag causes the loop cross section to expand radially outwards below the blob. If the magnetic field is strong enough, the resulting radial magnetic tension restoring force acts to counteract this and may even cause the rain blob to rebound several times near the footpoints (Mackay & Galsgaard 2001).
Antolin & Verwichte (2011) presented an observational study with Hinode/SOT in In Ca II H in which multiple coronal rain blobs are seen to oscillate transversely in phase. The oscillation periods lie between 100 s and 200 s with displacement amplitudes of the order of 500 km or less. It was concluded that the rain traces out a kink (Alfvénic) wave, either standing or running, supported by the whole coronal loop plasma (Nakariakov et al. 1999; Van Doorsselaere et al. 2008a; Goossens et al. 2009). For this event, the coronal rain acceleration, which has a value of 56 m s^{2} is also significantly subballistic. Kohutova & Verwichte (2016) detected two different regimes of transverse oscillations traced by the rain in a rain event observed by IRIS (De Pontieu et al. 2014): smallscale persistent oscillations driven by a continuously operating process and localised largescale oscillations excited by a transient mechanism. Transverse oscillations of coronal loops have frequently been observed in the EUV (e.g. Aschwanden et al. 1999, 2002; Wang & Solanki 2004; van Doorsselaere et al. 2008b; Verwichte et al. 2009; Aschwanden & Schrijver 2011; White & Verwichte 2012). Largeamplitude oscillations with displacements of several megameters are often excited impulsively by a nearby flare or CME (e.g. Aschwanden et al. 2002; Wang & Solanki 2004; De Moortel & Brady 2007; Van Doorsselaere et al. 2007; Verwichte et al. 2009, 2010; Mrozek 2011; White & Verwichte 2012), or directly by the reconnection process (White et al. 2012, 2013). The excitation mechanism of smallamplitude oscillations is less clear. Verwichte et al. (2004) reported oscillations in a postflare loop arcade that were driven by the motions of a nearby partially erupting prominence. Decayless or even growing continuous quasiperiodic oscillations have been reported and were associated with a lower atmosphere driver or nearby CME (Wang et al. 2012; Nisticò et al. 2013; Anfinogentov et al. 2015). Smallamplitude running transverse waves guided along the loops have been reported by Tomczyk et al. (2007), McIntosh et al. (2011), Threlfall et al. (2013). Smallamplitude oscillations are also often seen in coronal rain (Antolin & Verwichte 2011; Kohutova & Verwichte 2016). The potential of transverse waves for seismological probing of the coronal structure and magnetic field has been explored extensively (e.g. Nakariakov & Ofman 2001; Andries et al. 2009; Verth et al. 2010; Arregui & Asensio Ramos 2011; Goossens et al. 2012; Verwichte et al. 2013a,b; Pascoe et al. 2013).
Here we investigate the effect of the nonlinear ponderomotive force generated by a transverse oscillation (e.g. Allan 1993; Verwichte et al. 1999; Terradas & Ofman 2004) on the acceleration of coronal rain and evaluate its dependence on amplitude. Furthermore, we study the role of coronal rain in exciting transverse oscillations. In magnetohydrodynamics (MHD) a common definition of the ponderomotive force is as the nonlinear component of the Lorentz force along the equilibrium magnetic field resulting from the magnetic field perturbation of an oscillation or wave. Allan & Manuel (1996) demonstrated in a magnetospheric context that the ponderomotive force from MHD waves may transport plasma over large distances along the equilibrium magnetic field. They also suggested, without detail, that the ponderomotive force from Alfvén waves can be compared by analogy to the frictionless motion of beads along a transversely oscillating, stretched string. Verwichte (1999) has shown that up to third order in the normalised oscillation amplitude the modelling of the transverse wave using this mechanical analogue or using MHD are in agreement. We develop a 1.5 dimensional nonlinear mechanical model, which allows us to easily resolve both coronal blob kinematics and the transverse oscillation.
The paper is structured as follows. In Sect. 2 we present the mechanical model and derive the coupled system of differential equations for the rain kinematics and transverse wave field. In Sect. 3 we study the rain kinematics in the presence of a single oscillation harmonic under the assumption of negligible rain mass. In Sect. 4 we apply the model to an example observation set of coronal rain from Hinode/SOT. In Sect. 5 we model the excitation of the transverse oscillation by rain in an inclined loop. Finally, in Sect. 6 we discuss our findings.
2. Mechanical model
We model coronal rain as a single blob of mass m that is frozen in to the magnetic field line as a bead attached to a string. The magnetic field line has a semicircular shape with a major radius R and loop length L = πR. We neglect the transverse structuring for simplicity. The position of the blob is given by its position parallel to the magnetic field, s_{p}(t), and normal to the loop plane, x_{p}(t). We include gravity, which along the field line is of the form g(s) = g_{⊙}cos(s/R), where s is the independent coordinate along the loop. The displacement of the loop in the direction normal to the loop plane is given by ξ(s,t).
The Langrangian for this system is given by (1)where S is a constant loop cross section, ρ is the mass density of the coronal plasma, B is a uniform magnetic field strength, and μ_{0} is the permeability of free space. The integral term is the difference between the kinetic energy and potential energy of the transverse wave motion associated with the magnetic tension force. The second and third terms are the difference between the kinetic energy and gravitational potential energy of the rain blob. A constraint is added to ensure the blob remains on the field line, i.e. (2)This model is essentially onedimensional with propagation only along the magnetic field line. The fast magnetoacoustic and Alfvén waves are degenerate and both describe a transverse wave. Because we do not include transverse loop structuring, the typical wave phase speed is the Alfvén speed instead of the kink speed. For simplicity, we assume that there is no mass flux into or out of the loop. Then, the total loop mass M = m + LSρ is a constant. We introduce the dimensionless parameter (3)which ranges from zero (no coronal rain), to unity (half rain, half coronal plasma), to infinity (no coronal plasma). We find m/M = 0.2 and μ = 0.25 for coronal rain that is ten times denser than the coronal plasma and extending in length over 2 Mm in a 100 Mm loop (Antolin et al. 2010). If we independently include an additional reduction in crosssectional area for rain by a factor of say 36 to take the observed transverse fine structure into account (Antolin & Rouppe van der Voort 2012), we find a much lower value of m/M ≈ μ ≈ 0.01. On the other hand we may also consider modelling a complete rain shower (Antolin & Rouppe van der Voort 2012) event as a whole, for which the total mass ratio may be as high as unity (Antolin et al. 2015).
The equations of motion describing the transverse oscillation and the blob motion follow from minimising the functional (4)with respect to the dependent variables where λ is a Lagrangian multiplier. We also add a Rayleightype dissipative functional of the form (5)where τ represents a typical time over which transverse oscillation damp due to, for example, resonant absorption (Ruderman & Roberts 2002). This leads to the equations
and (8)The Alfvén speed of the coronal plasma is given by (9)The righthand side of Eq. (6) shows that a coronal rain blob feels two competing forces: a downwards pointing gravity and a ponderomotive force from the wave field.
If we assume that the blob is light so that μ≪ 1, then the wave is not modified by the presence of the blob and is readily described by the solution (10)where k = n/R, ω ≈ V_{A}k for weak damping and n is an integer. The equation of motion of the blob itself is then described by (11)where the subscript “p” has been dropped for simplicity and where
(12)with (13)For typical coronal conditions, with g_{⊙} = 274 m s^{2}, and assuming wave period and wavelengths of 300 s and 200 Mm, respectively, we find α = 0.08. Thus, an assumption of a regime of α ≪ 1 is reasonable. To leading order in a, the term a_{0} has a contribution to the blob acceleration from the transverse oscillation that does not vanish when averaging over a period of oscillation in the limit of no damping. This term represents a secular ponderomotive acceleration acting on the blob.
3. Coronal rain kinematics in presence of transverse oscillation
For our model, we consider the stationary points and their stability in the limit of τ → ∞. There is always a stationary point at the loop top, i.e. s = πR/ 2, where the gravitational acceleration along the field line is zero. In the absence of an oscillation (a = 0) any small displacement from the loop top would result in the blob falling in freefall to the solar surface. However, if the oscillation amplitude is large enough the ponderomotive force can balance gravity and the blob may remain suspended at or oscillate around the loop top. We consider that a,α ~ O(ϵ) where ϵ ≪ 1. The kinematics of the blob is modelled by the introduction of two timescales, i.e. t_{0} = t and t_{1} = ϵt, and an expansion of s = s_{0}(t_{0},t_{1}) + ϵ^{2}s_{2}(t_{0},t_{1}) (Nayfeh 2004). Equation (11) then reduces to orders O(1) and O(ϵ) to the conditions (14)which shows that s_{0} is only a function of t_{1}. The terms in Eq. (11) of O(ϵ^{2}) reduce to (15)where (16)Because U is not a function of time, the last term of Eq. (15) would lead to a secularly growing solution of s_{2}, unless the righthand side of Eq. (15) is zero. This leads to an evolutionary equation for s_{0} with respect to slow time t_{1} as follows:(17)which may be integrated to an energy balance equation, (18)where ℰ is a constant of integration that is determined by initial conditions. The function U fulfils the role of a potential. The solution of Eq. (15) is then (19)which shows that on top of the slow largescale dynamics of the blob there are small oscillations superimposed at half the oscillation period of the loop.
To understand the blob kinematics we study the topology of Eq. (18) in the phase space of s_{0} and . Critical points exist where the potential is extremal, i.e. , (20)or using a binomial expansion for the sine function on the lefthand side,
(21)This equation confirms that the loop top, i.e. s_{0} = πR/ 2, is always a critical point. In addition there are up to 2n more critical points. The nature of the critical points is determined by the sign of the second derivative of the potential, (22)with a positive (negative) sign corresponding to a centre (saddle point). The loop top is a centre only if n is an odd integer and (23)This condition is the minimum oscillation amplitude required to prevent the blob from falling. For typical coronal values of R = 50 Mm and V_{A} = 1000 km s^{1}, we find a_{crit} = 0.17/n, which corresponds to a loop displacement amplitude of 8/n Mm. Oscillations with such amplitudes have been observed by e.g. Hershaw et al. (2011). For the fundamental mode (n = 1), two other critical points exist if a>a_{crit}, (24)which can easily be verified to be saddle points. The phase diagram for n = 1 for the cases where a<a_{crit} and a>a_{crit} are illustrated in Fig. 1.
Fig. 1 Phase diagram associated with Eq. (17) and n = 1, for a<a_{crit} (top) and a>a_{crit} (middle). The solid line is the path of a blob with initial position s(0) = 0.45L and initial velocity v(0) = −10^{5}ω/k. The dashed line is the path of a blob with the same initial conditions in the absence of an oscillation (a = 0). The bottom panel shows the distance along loop of the blobs as a function of time for the three cases. 

Open with DEXTER 
Fig. 2 Same as Fig. 1 for n = 2. Because the mode frequency ω of the first overtone is twice that of the fundamental mode, the normalised ballistic fall time ωt_{fall} is double the value here compared with Fig. 1 whilst the actual time t_{fall} remains the same. 

Open with DEXTER 
Fig. 3 Fall time t_{max} relative to ballistic time t_{fall} as a function of (Ωτ)^{2} (Top). Coloured dots indicate cases whose paths are shown in the phase space diagram (middle) and in the timedistance plot (bottom). 

Open with DEXTER 
Fig. 4 Variance of Hinode/SOT intensity in the Ca II H band on the northeast limb on 16 April 2012 for the time period between 15:04 and 15:36 UT. Regions of high variability are dark. The path along the oscillating loop is indicated by two parallel dashed lines. 

Open with DEXTER 
Fig. 5 Relative intensity as a function of time relative to 15:04 UT and distance across the path for three positions along the path indicated in Fig. 4. 

Open with DEXTER 
Fig. 6 Relative intensity as a function of time relative to 15:04 UT and distance along the path. The intensity has been averaged across part of the path width. The dashed lines show the parallel position of five coronal rain blobs as a function of time. 

Open with DEXTER 
Fig. 7 Rain blob projected distance (top), speed (middle), and acceleration (bottom) as a function of time for five measured coronal rain blobs (error bars). The solid lines are polynomial fits to the measurements. The solid thin curves are numerically generated paths for blobs of negligible mass starting at s = 0.56L for amplitude a = 0.25 and initial parallel speeds of −20, −10, 0, 10, and 20 km s^{1}, respectively. The dashed thin curves are the equivalent for a = 0.025 and speeds −25, −20, and −15 km s^{1}. Time is measured relative to start time of the simulation. 

Open with DEXTER 
Fig. 8 Phase diagram of projected position vs. velocity for the 5 measured coronal rain blobs (in green). The solid green lines are polynomial fits to the measurements. The solid thin curves are numerically generated paths for blobs of negligible mass starting at random positions between 0.3L and 0.65L and speeds between −25 km s^{1} and 25 km s^{1} for amplitudes ranging from a = 0.01 to 0.5. 

Open with DEXTER 
Between the two saddle points, the blob may oscillate. The period of oscillation is found by expanding Eq. (17) around the loop top with s_{0} = πR/ 2 + δs, (25)where (26)For a = 0.2–0.5, the same typical coronal values as before, and a transverse oscillation period of 300 s we find a blob period in the range 900−3500 s. For fixed oscillation frequency ω, Ω is independent of the wave number n. Also, the maximum blob displacement is δs = Rarcsin(4α^{2}/a^{2}). The slow upanddown oscillation of the blob is a clear signature of the ponderomotive force acting on coronal rain blob in a coronal loop and is prescribed by the transverse loop oscillation amplitude and period.
For the first harmonic overtone (n = 2), the loop top is always a saddle point. However, there can exist centres near the maxima in the oscillation displacement halfway between footpoint and loop top. From Eq. (21), we obtain a thirdorder polynomial in sin(s_{0}/R), (27)which has three real solutions (a saddle point at the loop top and a centre in each loop leg) only if the discriminant is negative, i.e.(28)The value a_{crit} found here is similar to that for the centre at the loop top for a fundamental mode. The location of the two centres in the loop legs requires solving the thirdorder polynomial. From considering the two extreme cases of a = a_{crit} and a → ∞, we find that they are located within the intervals (29)We integrate Eq. (11) numerically using an explicit RungeKutta method at fourthorder accuracy (RK4). Figures 1 and 2 illustrate the kinematics of a rain blob in a transverse loop oscillation for τ → ∞. For a fundamental transverse oscillation with a<a_{crit}, the blob is seen falling to the photosphere at a subballistic rate. If a>a_{crit} and the initial speed is not large, then the ponderomotive force is strong enough to keep the blob oscillating around the loop top. The oscillation period is consistent with the analytical result given by Eq. (26). For a first overtone transverse oscillation a blob initially near the loop top falls superballistically in the top half of the loop because of the additional downwards acceleration from the ponderomotive force. The blob has then picked up enough speed to continue to the photosphere.
We now consider the transverse oscillation damping time, τ, to be finite. Then, an oscillation whose amplitude is above the critical value to keep a blob suspended, is not be able to keep the blob suspended indefinitely and once the amplitude drops below the critical value, the blob falls to the photosphere. Therefore, the number of turns the blob may complete in the phase diagram depends on the product Ωτ. Figure 3 illustrates the blob kinematics as a function of Ωτ. For a typical loop of radius R = 50 Mm, supporting a fundamental mode transverse loop oscillation with a period of 150 s and quality factor ωτ = 20, we have a_{crit} = 0.08. Then for a range of relative amplitude values a = 0.1, 0.2, 0.3, we find values for Ωτ = 0.9, 2.6, and 4.1, respectively. In terms of periods 2π/ Ω, it corresponds to values of 56 min, 19 min, and 12 min, respectively.
4. Modelling of observations of coronal rain oscillations
We examine observations of coronal rain that exhibits nonmonotonic kinematics in the presence of transverse oscillations in NOAA AR 11461 on the northeast limb in the Ca II H band of Hinode/SOT, taken on 16 April 2012 from 15:04 to 15:36 UT. The data has a spatial resolution of 0.22 arcsec and a time cadence of 24 s. Later from 17:24 UT onwards a large solar eruption takes place in the active region with an associated GOES class M1.7 flare that peaks at 17:45 UT. Transverse oscillations are excited in coronal loops in the vicinity. We examine one such loop in which coronal rain is present (see Fig. 4). We assume a semicircular, planar model for the loop with a radius of 45 Mm and an inclination of 30 degrees with respect to the photospheric normal. The loop length is estimated assuming a semicircular loop to be L = 140 Mm. It is reasonable to expect this loop length estimate to have a relative error of circa 20%. A region of interest is selected along a loop path in which coronal rain is visible. Figure 5 shows the relative intensity across this path at three locations near the loop top. Several coronal rain blobs are seen to oscillate transversely with a period of approximately three minutes.
The oscillation characteristics are found by applying the same analysis method as used by Antolin & Verwichte (2011). We observe the oscillation over approximately five periods. We find a mean oscillation period, P = 154 ± 20 s, and a mean transverse displacement amplitude, ξ_{0} = 1.1 ± 0.4 Mm. From this follows a projected transverse velocity amplitude, v_{⊥ 0} = 2πξ_{0}/P = 45 ± 20 km s^{1}. The oscillation has the largest displacement near the loop top. We therefore assume that the loop is mainly oscillating in the fundamental harmonic mode. The wave number, k = 1 /R = 0.022 ± 0.01 Mm^{1}. From this follows a relative oscillation amplitude a = ξ_{0}k = 0.025 ± 0.01.
Figure 6 shows the position of the coronal rain along the path as a function of time. Many coronal rain blobs are seen to be falling towards the solar surface nonmonotonically. The blobs are seen to oscillate up and down a few times during their descent with a “longitudinal” period P_{long} varying between 7 and 15 min. Four coronal rain blobs are tracked in time as a function of distance along the loop. Figure 7 shows their positions as a function time and the positionvelocity tracks in the phase diagram based on polynomial fits of the measurements. We focus on the coronal rain starting from near the loop top. We model the kinematics for a blob starting near the loop top for several initial speeds between −25 and 25 km s^{1} and for the observed amplitude a = 0.025. Also, a finite damping time, τ = 280 s, is included to allow us to model of rain falling nonmonotonically. Figure 7 shows that the numerically generated kinematics shows reasonable agreement with the observations in terms of fall times and speeds. But, importantly, to explain a longitudinal periodicity of 15 min for observed rain #1, i.e. Ω = 7 × 10^{3} rad s^{1}, we require a larger oscillation amplitude. Using Eq. (26), with g_{⊙} = 274 m s^{2}, we estimate a value of a = 0.26 (ξ_{0} = 11 Mm) is required to explain this periodicity. Figures 7 and 8 show that a good comparison is found for a = 0.25 and v_{0} = −25 km s^{1}. For the other initial velocities, the fall time is delayed by up to 30% compared with the observation of #1.
We consider two further observational studies of rain kinematics in the presence of transverse oscillations by Antolin & Verwichte (2011) and Kohutova & Verwichte (2016), where rain does not exhibit nonmonotonic kinematics, but we aim to model the subballistic fall. Antolin & Verwichte (2011) measured transverse rain oscillations with periods around 150 s and displacement amplitudes around 350 km in a loop estimated to be about 80 ± 15 Mm long. We forwardmodel rain kinematics for such a loop supporting undamped oscillations for a range of oscillation amplitudes. The highest value (shown in red) corresponds to 0.98a_{crit}. Figure 9 shows the kinematics for the projected speed and acceleration as a function of height for a loop of length 70 Mm. We chose a value of 70 Mm instead of 80 Mm as to be better able to directly compare with the results shown in Fig. 4 from Antolin & Verwichte (2011). With this approach we ignored the effects of projection and noncircularity on the measurements. In order to match measured speeds of 30−40 km s^{1}, the oscillation displacement amplitude has to be larger than 2.5 Mm, which is at least seven times the observed amplitude and is larger than the critical amplitude for which the model predicts that the rain does not fall but is trapped around the loop top. We also show the effective downwards acceleration, i.e. the average projected acceleration along the path, (30)In the absence of the ponderomotive force, the effective acceleration becomes the effective gravity, which for a circular loop is of the form ⟨ g_{⊙ eff} ⟩ = (2 /π)g_{⊙} = 174 m s^{2}. As Fig. 9 shows, a finite oscillation amplitude lowers the effective acceleration from ⟨ g_{eff} ⟩ for a = 0 to zero at a = a_{crit}. Antolin & Verwichte (2011) measured an effective acceleration centred on a mean value of 56 m s^{2}. In order to reproduce this value an oscillation displacement within a narrow range around 2.5 Mm is required.
Kohutova & Verwichte (2016) measured oscillations in a loop of length 129 Mm with periods around 200 s and displacement amplitudes of 200−400 km. From a similar analysis as performed for the previous observational study, we find that a displacement amplitude of at least 4 Mm, which is almost ten times the observed amplitudes, is required to explain the observations. Kohutova & Verwichte (2016) also found longperiod oscillation of periods around 17.4 min with a larger displacement of 1 Mm. However, since the main component of the ponderomotive force is proportional to ω^{2}, the required amplitude to achieve the same uplift increases. Therefore, the same analysis performed for this periodicity shows that a displacement amplitude exceeding 20 Mm is needed to explain the observed kinematics.
Fig. 9 Left and middle: simulated kinematics the height of rain blobs as a function of planeofthe sky projected speed for a range of transverse oscillations amplitudes for a circular loop of length 70 Mm. Kinematic tracks for different amplitudes are represented by different colours. The green area represents the subballistic regime. Right: effective acceleration as defined by Eq. (30) as a function of oscillation displacement amplitude. The effective gravity and critical displacement amplitude are highlighted. The solid curve is a best powerlaw fit within the constraints that it is equal to ⟨ g_{⊙ eff} ⟩ for a = 0 and 0 for a = a_{crit}. 

Open with DEXTER 
5. Excitation of transverse loop oscillations by coronal rain
We may extend the model to include an excitation mechanism for transverse oscillations by coronal rain of finite mass, i.e. μ finite. There are several possible excitation scenarios. First, through the curvature of the loop, the inertia of the rain creates a centrifugal acceleration that moves the coronal loop radially outwards. We expect predominately that the first overtone of a vertically polarised oscillation is excited. Since the mechanical model does not include curved geometry, we do not examine this scenario here. Second, through the gravitational acceleration of the rain mass, concentration on a coronal loop moves the loop downwards. The polarisation of the mode depends on the inclination of the loop with respect to the photospheric normal. We again expect again a vertically polarised mode in an uninclined loop. But with finite inclination the rain mass also moves the coronal loop sideways along with downwards. For a rain blob starting near the loop top, we then expect predominately that the horizontally polarised fundamental mode is excited. We can easily model the second scenario by extending the model to include a loop that is inclined by an angle θ with respect to the photospheric normal. For such a loop, the gravity vector may be decomposed into three components, i.e. (31)where 1_{∥}, 1_{⊥} and 1_{∧} form a coordinate triad and point radially and azimuthally in the loop plane, and normal to the plane, respectively (see Fig. 10). The governing wave equation for horizontally and vertically polarised oscillations become (32)where (33)and ξ_{∧} and ξ_{⊥} are the horizontally and vertically polarised displacements. respectively. Equation (32) is turned into a system of ordinary differential equations for each polarisation using a decomposition into spatial harmonics that satisfy the boundary conditions, (34)The delta function is likewise decomposed into (35)Equation (32) is decomposed into the system of ODEs (36)where (37)and (38)with Ĉ_{p} = (πp)^{1} if p is odd and Ĉ_{p} = 0 if p is even. Also, in keeping with the resonant absorption mechanism, τ_{n} = τ_{1}/n. The system of ODEs (Eq. (37)), together with Eq. (6), are numerically integrated for ξ_{n}(t) and the rain kinematics. To avoid an excitation of oscillations due to an instantaneous appearance of a coronal rain mass at t = 0, we include a ramp up of the mass of the rain over a typical time duration of t_{ramp} = 100 s, i.e. m(t) = m_{0}(1−exp(−t/t_{ramp})). In reality, the blob excites in both horizontal and vertical modes. For simplicity, in the modelling presented here we ignored the coupling between the two polarisation through the influence of the ponderomotive force on the blob kinematics.
Fig. 10 Model of an inclined loop with the decomposition gravity vector at the rain blob, where , and g_{⊙ , ∧} = −g_{⊙}sinθ1_{∧}. 

Open with DEXTER 
Fig. 11 Top: horizontally polarised wave field ξ_{∧} as a function of time and space for a coronal rain blob forming at s = 0.48L with a mass corresponding to μ = 0.25. The loop has length 100 Mm, Alfvén speed V_{A0} = 1000 km s^{1}, and an inclination of θ = 50°. Also, τ_{1} = 500 s and t_{ramp} = 100 s. The curve is the path s_{p}(t). Bottom: time evolution of the 5 first harmonic amplitudes ξ_{∧ ,n}. The dashed curves are the equivalent for τ_{1} → ∞ and t_{ramp} = 0 s. 

Open with DEXTER 
Fig. 12 Oscillation amplitude of the fundamental harmonic of a horizontally and vertically polarised transverse oscillation as a function of coronal rain mass m/M for the same loop as in Fig. 11 for several loop inclination angles and with τ_{1} → ∞ and t_{ramp} = 0 s. Initially the rain blob is located at 0.745L with zero speed. 

Open with DEXTER 
Figure 11 shows an example of the excitation of a transverse oscillation by the coronal rain by solving Eqs. (6) and (37) numerically for a typical coronal rain blob with mass m/M = 0.2 (μ = 0.25). It confirms that predominately the fundamental harmonic is excited. The blob is displaced down from the initial position with a superimposed oscillation. The displacement amplitude of the generated oscillation is of the order of 0.1−0.2% of loop length. For a loop of 100 Mm length, this corresponds to an amplitude of the order of hundreds of km. The exact value depends on the choice of damping time τ_{1} and rampup time t_{ramp}, where the largest amplitudes are found where these times are equal to infinity and zero.
Fig. 13 Rain mass ratio m/M as a function of loop inclination θ by applying Eqs. (39) to the three discussed observational studies. Thick solid (dashed) lines are for horizontally (vertically) polarised modes. The shaded areas are the onesigma errors. 

Open with DEXTER 
Figure 12 shows that the maximum displacement amplitude ξ_{1}, for a rain blob that falls from an initially stationary position near the loop top at 0.475L, is approximately linearly proportional to the coronal rain mass m/M and , i.e. (39)The exact values depend on the initial conditions, i.e. position and speed, of the rain blob, and decrease as the starting position moves down a loop leg. The vertically polarised mode has half the amplitude of the horizontally polarised mode. The displacement amplitude is of the order of several hundreds of km. This is roughly consistent with observed rain displacement amplitudes. Furthermore, when the displacement amplitude of a rain blob or shower is measured, the rain kinematics is understood, and the loop inclination is known, a seismological method is available to estimate the fraction of the rain mass relative to the hot loop mass.
Event parameters.
In Fig. 13 the Eqs. (39) are applied to the three previously examined observational studies, i.e. event of 16 April 2012, studies by Antolin & Verwichte (2011, hereafter A11) and Kohutova & Verwichte (2016, hereafter K16) using the relevant parameters as shown in Table 1. We assume that the simulated rain blob represents a rain shower. In all these studies the examined loops show small inclinations with respect to the photospheric normal of 30° or less. The smallamplitude horizontally polarised transverse oscillations observed by Kohutova & Verwichte (2016) could be explained by wave excitation provided the rain mass comprises at least 20−40% of the total loop mass. The oscillations observed by Antolin & Verwichte (2011) could marginally be explained by wave excitation but the rain mass would have to comprise at least 60−80% of the total loop mass. The event of 16 April 2012 and the longperiod oscillations seen by Kohutova & Verwichte (2016) can be ruled out to be excited by the rain because they would require a rain mass that is unrealistically high, i.e. close to or even exceeding 100% of the total loop mass.
6. Discussion
We have studied the kinematics of coronal rain in the presence of a transversely oscillating loop using an analytical model of a rain blob guided by the coronal magnetic field as the mechanical analogue of a moving point mass on an oscillating string with gravity. The ponderomotive force from the shear oscillation pushes rain blobs towards the antinodes in their displacement field. A fundamental mode creates an additional force besides gravity acting on coronal rain towards the loop top. The fall of coronal rain is thus becoming subballistic. If a critical oscillation amplitude is exceeded, the rain does not fall at all but oscillates slowly up and down around the loop top. If the oscillation is damped, this motion is temporary and as soon as the amplitude goes below the critical amplitude, the rain eventually falls towards the surface. We sought to identify these characteristics in several observational studies of coronal rain in the presence of transverse oscillations. We found that upanddown motions of coronal rain is indeed seen. In one study we found that though we can explain the observed rain speeds, the amplitude necessary to explain the long periodicity is about ten times larger than what is observed. It is not likely that this discrepancy can be understood by a lineofsight effect of the plane of polarisation of the oscillation. We investigated two further observational studies where subballistic rain is seen in the presence of oscillations. We found that the required amplitude also tends to be about an order of magnitude higher than what is observed. Therefore, the ponderomotive force is not likely to be the primary physical reason for subballistic fall of coronal rain in most cases. But this is not surprising since subballistic motion has been observed in the absence of any oscillations. This study, however, allows us to evaluate the contribution from the ponderomotive force on coronal rain kinematic.
The model also allows us to study the excitation of transverse oscillations by the presence of the coronal rain mass in a loop under the influence of solar gravity. The appearance of a cold localised mass displaces the loop downwards. This sets up a transverse oscillation in the loop. Its amplitude depends on the mass ratio between rain and hot loop plasma, the inclination of the loop with respect to the photospheric normal, the timescale at which the rain forms, and the inertia. The fundamental mode is predominately excited with predicted displacement amplitudes in the range of hundreds of km for rain forming near the loop top. This is in the range of those often observed. In fact, we may explain the shortperiod oscillations reported by Kohutova & Verwichte (2016) as rainexcited provided the rain mass comprises at least 20−40% of the total loop mass. For other events, the required rain mass may be too high or impossible. However, Antolin et al. (2015) have shown that in some cases rain showers may make up most of the mass of the loop. Also, the vertically polarised mode has a predicted amplitude that is half that of a horizontally polarised mode (at θ = 45°). The presence of coronal rain in loops may be an important mechanism for exciting transverse oscillations.
The analytical model is limited in that it does not take the roles of plasma thermodynamics, pressure, or transverse structuring into account. Detailed numerical nonlinear MHD simulations will be undertaken to obtain a fuller picture of the relationship between transverse oscillations and coronal rain. However, this study will help to recognise those features in the simulations arising from the ponderomotive action or wave excitation.
Acknowledgments
E.V. acknowledges support from the Warwick STFC Consolidated Grant ST/L000733/I. P.A. acknowledges support from the EU Horizon 2020 Research and Innovation programme (grant agreement No. 647214). P.K. acknowledges support from a UK STFC Ph.D. studentship. T.N. acknowledges support from the St Andrews STFC Consolidated Grant SN/N000609/1. Hinode is a Japanese mission developed and launched by ISAS/JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). The work was also supported by the international programme “Implications for coronal heating and magnetic fields from coronal rain observations and modelling” of the International Space Science Institute (ISSI), Bern. This research has made use of SunPy, an opensource and free communitydeveloped solar data analysis package written in Python (http://sunpy.org).
References
 Ahn, K., Chae, J., Cho, K.S., et al. 2014, Sol. Phys., 289, 4117 [NASA ADS] [CrossRef] [Google Scholar]
 Allan, W. 1993, J. Geophys. Res., 98, 1409 [NASA ADS] [CrossRef] [Google Scholar]
 Allan, W., & Manuel, J. R. 1996, Annales Geophysicae, 14, 893 [NASA ADS] [CrossRef] [Google Scholar]
 Andries, J., Van Doorsselaere, T., Roberts, B., et al. 2009, Space Sci. Rev., 149, 3 [NASA ADS] [CrossRef] [Google Scholar]
 Anfinogentov, S. A., Nakariakov, V. M., & Nisticò, G. 2015, A&A, 583, A136 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Antolin, P., & Rouppe van der Voort, L. 2012, ApJ, 745, 152 [NASA ADS] [CrossRef] [Google Scholar]
 Antolin, P., & Verwichte, E. 2011, ApJ, 736, 121 [NASA ADS] [CrossRef] [Google Scholar]
 Antolin, P., Shibata, K., & Vissers, G. 2010, ApJ, 716, 154 [NASA ADS] [CrossRef] [Google Scholar]
 Antolin, P., Vissers, G., Pereira, T. M. D., Rouppe van der Voort, L., & Scullion, E. 2015, ApJ, 806, 81 [NASA ADS] [CrossRef] [Google Scholar]
 Arregui, I., & Asensio Ramos, A. 2011, ApJ, 740, 44 [NASA ADS] [CrossRef] [Google Scholar]
 Aschwanden, M. J., & Schrijver, C. J. 2011, ApJ, 736, 102 [NASA ADS] [CrossRef] [Google Scholar]
 Aschwanden, M. J., Fletcher, L., Schrijver, C. J., & Alexander, D. 1999, ApJ, 520, 880 [NASA ADS] [CrossRef] [Google Scholar]
 Aschwanden, M. J., de Pontieu, B., Schrijver, C. J., & Title, A. M. 2002, Sol. Phys., 206, 99 [NASA ADS] [CrossRef] [Google Scholar]
 Athay, R. G., White, O. R., Lites, B. W., & Bruner, Jr., E. C. 1980, Sol. Phys., 66, 357 [NASA ADS] [CrossRef] [Google Scholar]
 De Groof, A., Berghmans, D., van DrielGesztelyi, L., & Poedts, S. 2004, A&A, 415, 1141 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 De Groof, A., Bastiaensen, C., Müller, D. A. N., Berghmans, D., & Poedts, S. 2005, A&A, 443, 319 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 De Moortel, I., & Brady, C. S. 2007, ApJ, 664, 1210 [NASA ADS] [CrossRef] [Google Scholar]
 De Pontieu, B., Title, A. M., Lemen, J. R., et al. 2014, Sol. Phys., 289, 2733 [NASA ADS] [CrossRef] [Google Scholar]
 Fang, X., Xia, C., & Keppens, R. 2013, ApJ, 771, L29 [NASA ADS] [CrossRef] [Google Scholar]
 Fang, X., Xia, C., Keppens, R., & Van Doorsselaere, T. 2015, ApJ, 807, 142 [NASA ADS] [CrossRef] [Google Scholar]
 Goossens, M., Terradas, J., Andries, J., Arregui, I., & Ballester, J. L. 2009, A&A, 503, 213 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Goossens, M., Soler, R., Arregui, I., & Terradas, J. 2012, ApJ, 760, 98 [NASA ADS] [CrossRef] [Google Scholar]
 Hershaw, J., Foullon, C., Nakariakov, V. M., & Verwichte, E. 2011, A&A, 531, A53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Kawaguchi, I. 1970, PASJ, 22, 405 [NASA ADS] [Google Scholar]
 Kleint, L., Antolin, P., Tian, H., et al. 2014, ApJ, 789, L42 [NASA ADS] [CrossRef] [Google Scholar]
 Klimchuk, J. A., Patsourakos, S., & Cargill, P. J. 2008, ApJ, 682, 1351 [NASA ADS] [CrossRef] [Google Scholar]
 Kohutova, P., & Verwichte, E. 2016, ApJ, 827, 39 [NASA ADS] [CrossRef] [Google Scholar]
 Leroy, J.L. 1972, Sol. Phys., 25, 413 [NASA ADS] [CrossRef] [Google Scholar]
 Levine, R. H., & Withbroe, G. L. 1977, Sol. Phys., 51, 83 [NASA ADS] [CrossRef] [Google Scholar]
 Luna, M., Karpen, J. T., & DeVore, C. R. 2012, ApJ, 746, 30 [NASA ADS] [CrossRef] [Google Scholar]
 Mackay, D. H., & Galsgaard, K. 2001, Sol. Phys., 198, 289 [NASA ADS] [CrossRef] [Google Scholar]
 McIntosh, S. W., de Pontieu, B., Carlsson, M., et al. 2011, Nature, 475, 477 [NASA ADS] [CrossRef] [Google Scholar]
 Mrozek, T. 2011, Sol. Phys., 270, 191 [NASA ADS] [CrossRef] [Google Scholar]
 Müller, D. A. N., Hansteen, V. H., & Peter, H. 2003, A&A, 411, 605 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Müller, D. A. N., De Groof, A., Hansteen, V. H., & Peter, H. 2005, A&A, 436, 1067 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Nakariakov, V. M., & Ofman, L. 2001, A&A, 372, L53 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Nakariakov, V. M., Ofman, L., Deluca, E. E., Roberts, B., & Davila, J. M. 1999, Science, 285, 862 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Nayfeh, A. 2004, Perturbation Methods (John Wiley and Sons) [Google Scholar]
 Nisticò, G., Nakariakov, V. M., & Verwichte, E. 2013, A&A, 552, A57 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Oliver, R., Soler, R., Terradas, J., Zaqarashvili, T. V., & Khodachenko, M. L. 2014, ApJ, 784, 21 [NASA ADS] [CrossRef] [Google Scholar]
 Pascoe, D. J., Hood, A. W., De Moortel, I., & Wright, A. N. 2013, A&A, 551, A40 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Ruderman, M. S., & Roberts, B. 2002, ApJ, 577, 475 [NASA ADS] [CrossRef] [Google Scholar]
 Scharmer, G. B., Bjelksjo, K., Korhonen, T. K., Lindberg, B., & Petterson, B. 2003, in SPIE Conf. Ser. 4853, eds. S. L. Keil, & S. V. Avakyan, 341 [Google Scholar]
 Scharmer, G. B., Narayan, G., Hillberg, T., et al. 2008, ApJ, 689, L69 [NASA ADS] [CrossRef] [Google Scholar]
 Schrijver, C. J. 2001, ApJ, 547, 475 [NASA ADS] [CrossRef] [Google Scholar]
 Straus, T., Fleck, B., & Andretta, V. 2015, A&A, 582, A116 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Terradas, J., & Ofman, L. 2004, ApJ, 610, 523 [NASA ADS] [CrossRef] [Google Scholar]
 Threlfall, J., De Moortel, I., McIntosh, S. W., & Bethge, C. 2013, A&A, 556, A124 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Tomczyk, S., McIntosh, S. W., Keil, S. L., et al. 2007, Science, 317, 1192 [NASA ADS] [CrossRef] [PubMed] [Google Scholar]
 Tsuneta, S., Ichimoto, K., Katsukawa, Y., et al. 2008, Sol. Phys., 249, 167 [NASA ADS] [CrossRef] [Google Scholar]
 Van Doorsselaere, T., Nakariakov, V. M., & Verwichte, E. 2007, A&A, 473, 959 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Van Doorsselaere, T., Nakariakov, V. M., & Verwichte, E. 2008a, ApJ, 676, L73 [NASA ADS] [CrossRef] [Google Scholar]
 Van Doorsselaere, T., Nakariakov, V. M., Young, P. R., & Verwichte, E. 2008b, A&A, 487, L17 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Vashalomidze, Z., Kukhianidze, V., Zaqarashvili, T. V., et al. 2015, A&A, 577, A136 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Verth, G., Terradas, J., & Goossens, M. 2010, ApJ, 718, L102 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E. 1999, Ph.D. Thesis, The Open University [Google Scholar]
 Verwichte, E., Nakariakov, V. M., & Longbottom, A. W. 1999, J. Plasma Phys., 62, 219 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Nakariakov, V. M., Ofman, L., & Deluca, E. E. 2004, Sol. Phys., 223, 77 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Aschwanden, M. J., Van Doorsselaere, T., Foullon, C., & Nakariakov, V. M. 2009, ApJ, 698, 397 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Foullon, C., & Van Doorsselaere, T. 2010, ApJ, 717, 458 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Van Doorsselaere, T., Foullon, C., & White, R. S. 2013a, ApJ, 767, 16 [NASA ADS] [CrossRef] [Google Scholar]
 Verwichte, E., Van Doorsselaere, T., White, R. S., & Antolin, P. 2013b, A&A, 552, A138 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wang, T. J., & Solanki, S. K. 2004, A&A, 421, L33 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 Wang, T., Ofman, L., Davila, J. M., & Su, Y. 2012, ApJ, 751, L27 [NASA ADS] [CrossRef] [Google Scholar]
 White, R. S., & Verwichte, E. 2012, A&A, 537, A49 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 White, R. S., Verwichte, E., & Foullon, C. 2012, A&A, 545, A129 [NASA ADS] [CrossRef] [EDP Sciences] [Google Scholar]
 White, R. S., Verwichte, E., & Foullon, C. 2013, ApJ, 774, 104 [NASA ADS] [CrossRef] [Google Scholar]
All Tables
All Figures
Fig. 1 Phase diagram associated with Eq. (17) and n = 1, for a<a_{crit} (top) and a>a_{crit} (middle). The solid line is the path of a blob with initial position s(0) = 0.45L and initial velocity v(0) = −10^{5}ω/k. The dashed line is the path of a blob with the same initial conditions in the absence of an oscillation (a = 0). The bottom panel shows the distance along loop of the blobs as a function of time for the three cases. 

Open with DEXTER  
In the text 
Fig. 2 Same as Fig. 1 for n = 2. Because the mode frequency ω of the first overtone is twice that of the fundamental mode, the normalised ballistic fall time ωt_{fall} is double the value here compared with Fig. 1 whilst the actual time t_{fall} remains the same. 

Open with DEXTER  
In the text 
Fig. 3 Fall time t_{max} relative to ballistic time t_{fall} as a function of (Ωτ)^{2} (Top). Coloured dots indicate cases whose paths are shown in the phase space diagram (middle) and in the timedistance plot (bottom). 

Open with DEXTER  
In the text 
Fig. 4 Variance of Hinode/SOT intensity in the Ca II H band on the northeast limb on 16 April 2012 for the time period between 15:04 and 15:36 UT. Regions of high variability are dark. The path along the oscillating loop is indicated by two parallel dashed lines. 

Open with DEXTER  
In the text 
Fig. 5 Relative intensity as a function of time relative to 15:04 UT and distance across the path for three positions along the path indicated in Fig. 4. 

Open with DEXTER  
In the text 
Fig. 6 Relative intensity as a function of time relative to 15:04 UT and distance along the path. The intensity has been averaged across part of the path width. The dashed lines show the parallel position of five coronal rain blobs as a function of time. 

Open with DEXTER  
In the text 
Fig. 7 Rain blob projected distance (top), speed (middle), and acceleration (bottom) as a function of time for five measured coronal rain blobs (error bars). The solid lines are polynomial fits to the measurements. The solid thin curves are numerically generated paths for blobs of negligible mass starting at s = 0.56L for amplitude a = 0.25 and initial parallel speeds of −20, −10, 0, 10, and 20 km s^{1}, respectively. The dashed thin curves are the equivalent for a = 0.025 and speeds −25, −20, and −15 km s^{1}. Time is measured relative to start time of the simulation. 

Open with DEXTER  
In the text 
Fig. 8 Phase diagram of projected position vs. velocity for the 5 measured coronal rain blobs (in green). The solid green lines are polynomial fits to the measurements. The solid thin curves are numerically generated paths for blobs of negligible mass starting at random positions between 0.3L and 0.65L and speeds between −25 km s^{1} and 25 km s^{1} for amplitudes ranging from a = 0.01 to 0.5. 

Open with DEXTER  
In the text 
Fig. 9 Left and middle: simulated kinematics the height of rain blobs as a function of planeofthe sky projected speed for a range of transverse oscillations amplitudes for a circular loop of length 70 Mm. Kinematic tracks for different amplitudes are represented by different colours. The green area represents the subballistic regime. Right: effective acceleration as defined by Eq. (30) as a function of oscillation displacement amplitude. The effective gravity and critical displacement amplitude are highlighted. The solid curve is a best powerlaw fit within the constraints that it is equal to ⟨ g_{⊙ eff} ⟩ for a = 0 and 0 for a = a_{crit}. 

Open with DEXTER  
In the text 
Fig. 10 Model of an inclined loop with the decomposition gravity vector at the rain blob, where , and g_{⊙ , ∧} = −g_{⊙}sinθ1_{∧}. 

Open with DEXTER  
In the text 
Fig. 11 Top: horizontally polarised wave field ξ_{∧} as a function of time and space for a coronal rain blob forming at s = 0.48L with a mass corresponding to μ = 0.25. The loop has length 100 Mm, Alfvén speed V_{A0} = 1000 km s^{1}, and an inclination of θ = 50°. Also, τ_{1} = 500 s and t_{ramp} = 100 s. The curve is the path s_{p}(t). Bottom: time evolution of the 5 first harmonic amplitudes ξ_{∧ ,n}. The dashed curves are the equivalent for τ_{1} → ∞ and t_{ramp} = 0 s. 

Open with DEXTER  
In the text 
Fig. 12 Oscillation amplitude of the fundamental harmonic of a horizontally and vertically polarised transverse oscillation as a function of coronal rain mass m/M for the same loop as in Fig. 11 for several loop inclination angles and with τ_{1} → ∞ and t_{ramp} = 0 s. Initially the rain blob is located at 0.745L with zero speed. 

Open with DEXTER  
In the text 
Fig. 13 Rain mass ratio m/M as a function of loop inclination θ by applying Eqs. (39) to the three discussed observational studies. Thick solid (dashed) lines are for horizontally (vertically) polarised modes. The shaded areas are the onesigma errors. 

Open with DEXTER  
In the text 