A&A 395, 293-296 (2002)
DOI: 10.1051/0004-6361:20021355
P. F. Moretti1 - A. Cacciani2
- A. Hanslmeier3 - M. Messerotti4
- W. Otruba 5
- W. P
tzi5 - A. Warmuth3
1 - I.N.A.F., Osservatorio Astronomico di Capodimonte, Via Moiarello 16, 80131 Napoli, Italy
2 -
Department of Physics University of Rome, P.le A. Moro 2, 00185 Rome, Italy
3 - Institute of Geophysics, Astrophysics and Meteorology of the University of
Graz, Universitaetsplatz 5, 8010 Graz, Austria
4 - I.N.A.F., Osservatorio Astronomico
di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy
5 - Kanzelh
he Solar Observatory, 9521 Treffen, Austria
Received 13 November 2001 / Accepted 4 September 2002
Abstract
The presence of a solar background in the phase difference between the
intensity and velocity (I-V) p-mode oscillation signals recently has been
interpreted in terms of downflows due to convection (Skartlien & Rast 2000)
or due to chromospheric explosive events (Moretti et al. 2001a). In
support of the latter, we present I and V characteristics of impulsive
brightenings observed in the NaI D lines, show that these reproduce the
frequency dependence of the I-V modulation background, and show that
explanations invoking more frequently occurring phenomena such as seismic events are
not likely in low-l modulation data.
Key words: Sun: oscillations - Sun: flares
The presence of a background in the spectra of the phase difference between the solar intensity and velocity oscillation signals (I-V) was first discovered in ground observations by Deubner et al. (1990) as a negative phase "plateau'' between f=1 and f=2 mHz frequencies and at l values between 100 and 1000 (where l is the azimuthal mode number).
The initial explanation given by Deubner et al. (1992,
cf. Marmolino & Severino 1991; Marmolino et al. 1993) proposed a superposition
of downward and upward waves. Such a superposition reproduces the observed
frequency and height dependences of the I-V phase difference background fairly
well, but it requires low-frequency wave sources and reflections that have not
yet been identified.
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Figure 1:
A selection of the intensity (top), velocity (center) and
longitudinal magnetic field maps (bottom) obtained on 1 June 2000 in the NaI D
lines. Time goes from left to right in 2-min steps starting from 07:25:57
UT. Velocity is black if downward. A
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Figure 2:
The observed one-minute cadence intensity (top panel, solid) and
velocity (center panel, solid) on a
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Figure 3:
Left, from top to bottom a-d) a simulation at 1 minute cadence
of the intensity and velocity impulses a), the power spectra of the signals
b) and the intensity-velocity phase spectrum c) for a 9h zero-padded
time-series. d) the observed phase spectra at l=100 for the NaI D lines
obtained with 256 min runs at Naples (crosses) and Kanzelh
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Recently, Skartlien & Rast (2000) have proposed that the I-V phase difference background is dominated by localised sudden convective downflows corresponding to the "acoustic events'' observed by Espagnet et al. (1996), Goode et al. (1998), Strous et al. (2000), and thought to represent the principal sources of the global p-mode oscillations (Goode et al. 1998). Note, however, that Skartlien & Rast (2000) base this proposal on the I-V signature of a single event. We show below that the detectability in low-l oscillation measurements of the phase of many such events could be similar to that of other events whose contribution in the IV cross-spectrum is comparable.
A totally different explanation of the I-V phase difference background was recently forwarded by Moretti et al. (2001a), proposing that downward directed plasma jets due to explosive events in the upper solar atmosphere contribute to the observed I-V signatures in the photosphere.
In this paper we add further evidence for an explosive-event explanation of the I-V modulation background between f=1 and f=2 mHz and at low-ls by analysing the I-V phase behaviour of observed impulsive brightenings of the NaI D lines. The observations are described in Sect. 2. We then construct a model describing the phase difference signature of many such impulsive events (Sect. 3). We show that, at the NaI D line formation layers, the signature in low-l data of such impulsive events at the global occurrence rates of the explosive events in the chromosphere is dominant. We suspect that these are indeed related phenomena.
Many impulsive brightenings in the NaI D lines have been detected at the Solar Kanzelh
he
Observatory (Warmuth et al. 2000; Moretti et al. 2001b).
The data consist of intensity, velocity and longitudinal magnetic field
full-disk images acquired at one-minute intervals through a magneto-optical
filter (Cacciani et al. 1999; Cacciani et al. 1997). The spatial
resolution is
per pixel. Our results are reliable for
values between 20 and 400. The data have been calibrated as shown in Moretti
and the MOF Development Group (2000) and Cacciani & Moretti (1997).
A number of 25 min long I, V and B sequences were selected containing impulsive
brightenings respectively for April 2, June 1 and 6, July 12, 17, 19 and 22,
and September 12, 2001. High resolution ultraviolet spectra of the outer solar
atmosphere show transient brightenings often referred to as explosive
events. These explosive events have also been detected in Hobservations (Canfield & Metcalf 1987; Chae et al. 1998). These are localised
regions of small spatial extent that show sudden enhancements in the
intensities in the lines accompanied by strong non-Gaussian profiles (Sarro et al. 1999; Berghmans et al. 1998).
The physical mechanisms advanced
to explain these phenomena depend on the observed velocities, momentum,
energy etc. The explosive chromospheric evaporation model (Fisher et al.
1985) explains the main observed characteristics of those events whose spatial
scales are of the order of a few arcsec and last for a few minutes
(Canfield et al. 1987; Canfield & Metcalf 1987). The same scales are those
obtained by the analysis of the background locations maintaining spatial resolution
(Moretti et al. 2001a). Recently, observations in H
and NaI D lines
have shown a simultaneous occurrence of the impulsive brightenings (Warmuth et al. 2000; Moretti et al. 2001b). For this reason we suggest the impulsive
brightenings are related to the explosive events in the upper
atmosphere.
Due to the geometrical asymmetry and the complexity of the
structures, the contribution of the impulsive event in the velocity signal from
the surrounding oscillations is often difficult, since they are comparable (of
the order of some hundreds of m/s at these solar heights). We have chosen the
case of June 1 2001 as the clearest and simplest example of the induced
perturbations. Figure 1 shows partial regions of the I, V and Bsequences. Figure 2 shows the intensity and velocity behaviour with time for
the brightest pixel in Fig. 1.
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Figure 4:
Class prototype impulses randomly distributed in time and space as
described in Fig. 3 have been added and the resulting power spectrum for the
velocity signal is shown for a 40-1 global-sun occurrence. A one-month GONG
spectrum for ![]() ![]() ![]() ![]() |
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In low-l or full-disk helioseismology using long observing time-series, many impulsive events such as the one displayed in Fig. 2 are averaged. The characteristic I-V phase of such events may survive such averaging if it dominates over other signals. Since our data do not permit us to clearly separate the impulsive velocity signal from the global oscillation signals, the question arises whether impulsive event phase differences as in Fig. 2 contribute significantly to long-duration large-area I-V phase difference measurements.
We address this issue by using a model event shown in Fig. 3. The intensity peak has a duration similar to the pulse in Fig. 2. The velocity pulse describes downflow with a time profile that generates I-V phase differences close to those of the actual observations in the bottom panel of Fig. 3.
We use this model event as a prototype and compute the velocity power spectra after superposition of many such events, randomly distributed in space and time over the whole solar surface.
Dopplergrams every second at an 8 arcsec/pixel sampling and 60 s acquisition
time (as GONG does) have been obtained, and each
coefficient's time
series and its power spectrum have been computed.
A 40 s-1 global sun occurrence has been chosen as the one
reported for the chromospheric explosive events by Berghmans et al.
(1988).
The downflowing plasma jets we observed at the NaI D line formation
layers have not yet been detected at the lower photospheric heights such as
those investigated with the GONG data (with the exception of the high
energy event reported by Kosovichev & Zharkova 1998). For
this reason, we use reduced peak values for the prototype event: of
-50 m/s and 0.1 excess for velocity and intensity signals respectively.
The resulting power is comparable with that observed by GONG (see Fig. 4 for ).
Even if seismic events have a 4000 s-1 global sun occurrence,
their spatially averaged intensity and velocity signals are comparable to or
lower than those estimated for the impulsive events and their typical area extension
is at least 10 times smaller (Strous et al. 2000).
This implies that the detection of the phase of the seismic events should compete
with that of the impulsive brightenings.
At higher layers, where the seismic events are not detected, the impulsive brightenings events do dominate in the low frequency phase spectrum.
In this paper we show how the perturbations induced by the impulsive
events detected in the NaI D lines can reproduce the low frequency behaviour of
the solar I-V phase background and that this contribution is more likely to
furnish the Fourier power background in the low-
measurements employed in
helioseismology than the acoustic events described by Goode et al. (1998).
Acknowledgements
P.F.M. thanks Federica Brandizzi. We thank the referee for valuable help in preparing this paper. We also thank V. Andretta, S. M. Jefferies, G. Severino and the Solar Group of the OAC for fruitful discussion.
We thank Jim Pintar for the GONG data product obtained by the Global Oscillation Network Group (GONG) project, managed by the National Solar Observatory, which is operated by AURA, Inc. under a cooperative agreement with the National Science Foundation