Mesospheric bores at southern midlatitudes observed by ISS-IMAP/VISI: a first report of an undulating wave front

Large-scale spatial structures of mesospheric bores were observed by the Visible and near-Infrared Spectral Imager (VISI) of the ISS-IMAP mission (Ionosphere, Mesosphere, upper Atmosphere and Plasmasphere mapping mission from the International Space Station) in the mesospheric O₂ airglow at 762 nm wavelength. Two mesospheric bore events in southern midlatitudes are reported in this paper: one event at 48–54^∘ S, 10–20^∘ E on 9 July 2015 and the other event at 35–43^∘ S, 24^∘ W–1^∘ E on 7 May 2013. For the first event, the temporal evolution of the mesospheric bore was investigated from the difference of two observations in consecutive passes. The estimated eastward speed of the bore is 100 m s⁻¹. The number of trailing waves increased with a rate of 3.5 waves h⁻¹. Anticlockwise rotation with a speed of 20^∘ h⁻¹ was also recognized. These parameters are similar to those reported by previous studies based on ground-based measurements, and the similarity supports the validity of VISI observation for mesospheric bores. For the second event, VISI captured a mesospheric bore with a large-scale and undulating wave front. The horizontal extent of the wave front was 2200 km. The long wave front undulated with a wavelength of 1000 km. The undulating wave front is a new feature of mesospheric bores revealed by the wide field of view of VISI. We suggest that nonuniform bore propagating speed due to inhomogeneous background ducting structure might be a cause of the undulation of the wave front. Temperature measurements from the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) onboard the Thermosphere, Ionosphere, Mesosphere, Energetics and Dynamics (TIMED) satellite indicated that bores of both events were ducted in a temperature inversion layer.

1 Introduction

A mesospheric bore is characterized by a propagating and sharp front in the upper mesosphere. The front is often followed by undulations (undular bore) or turbulence (turbulent bore). Mesospheric bores have been observed as a sharp brightness jump or drop of airglow by ground-based imagers at various longitudes from low latitude to high latitude (Fechine et al., 2005; Li et al., 2013; Medeiros et al., 2018; Nielsen et al., 2006; Smith et al., 2003, 2017; Taylor et al., 1995).

Dewan and Picard (1998) proposed an explanation of mesospheric bores as a propagating discontinuity in a stable layer or a duct in varicose mode. In varicose mode, the upper and lower surfaces of the layer oscillate symmetrically about the mid-plane. Medeiros et al. (2005) demonstrated that most bores showed the complementary effect suggested by Dewan and Picard (1998) in airglow responses, and validated the varicose-mode oscillation. By solving conservation of mass and momentum equations, Dewan and Picard (1998) calculated the speed of a bore as follows:

$$\begin{array}{}\text{(1)}& {\displaystyle }U=\sqrt{g^{\prime }{\displaystyle \frac{h_{\mathrm{1}}(h_{\mathrm{1}}+h_{\mathrm{0}})}{\mathrm{2}{h}_{\mathrm{0}}}}}.\end{array}$$

Here, h₀ and h₁ are the half width of a ducting layer upward and downward of a bore, respectively; g^′ is the gravitational acceleration corrected for buoyancy force. The mesospheric bore model in a thermal duct has been examined and validated using simultaneous lidar and airglow imager observations (She et al., 2004; Smith et al., 2003, 2005). It has been also demonstrated with simultaneous radar observations that wind has an important role in the background condition of mesospheric bores (Fechine et al., 2009; Giongo et al., 2018). Dewan and Picard (2001) provided a possible explanation of mesospheric bores through the critical layer interaction of gravity waves with the mean flow. Seyler (2005) and Laughman et al. (2009) demonstrated, by using a numerical simulation, that a wave front of a long-wavelength gravity wave in a duct can steepen and become a bore-like sharp front. Such a formation of a mesospheric bore from large-scale gravity waves was reported by Yue et al. (2010) utilizing ground-based observations. However, the generation mechanism of mesospheric bores is still not fully understood.

Historically, the study of mesospheric bores has been conducted based on ground-based measurements. Recently, Miller et al. (2015) reported two space-borne observations of mesospheric bore events by Day/Night Band (DNB) onboard the NOAA/NASA Suomi National Polar-orbiting Partnership environmental satellite. Although there are successful observations of mesospheric bores by DNB, a lot of work is left to do on the study of mesospheric bores with space-borne imaging. First, the geographical variation of the bore characteristics is not fully understood. The number of ground-based observation sites is limited, and the locations of observation sites are restricted by land–sea distribution. There are reports of bore observations at low latitudes (Fechine et al., 2005; Medeiros et al., 2001, 2018), northern midlatitudes (Li et al., 2013; Smith et al., 2003, 2017; Taylor et al., 1995), and southern high latitudes (Li et al., 2013; Medeiros et al., 2018; Nielsen et al., 2006), but there are no reports in southern midlatitudes and northern high latitudes. Second, the large-scale horizontal structure of bores is unclear. Since ground-based imagers have often observed only a portion of a bore's wave front, the typical horizontal spatial scale of mesospheric bore seems to be larger than the imager's field of view (FOV). Previous studies based on ground-based observations have provided limited information on a bore's large-scale horizontal structure. Space-borne airglow imaging is a strong tool to study mesospheric bores with global observational coverage and a wider FOV, and can overcome the limitations of ground-based observations.

The Visible and near-Infrared Spectral Imager (VISI) of the ISS-IMAP mission (Ionosphere, Mesosphere, upper Atmosphere and Plasmasphere mapping mission from the International Space Station) is another instrument that has a capability of imaging mesospheric airglow from space with a wide FOV. While Miller et al. (2015) limited their focus to illustrating the DNB's potential for bore observation, we report two successful bore events from VISI with further detailed analyses to address two topics: the latitudinal difference of the bore characteristics and the large horizontal structure. In this paper, we report two mesospheric bores observed by VISI at southern midlatitudes. The bore of event no. 1 was captured in two consecutive passes by VISI; thus, the temporal evolution of the structure can be investigated from the difference of two images. The bore showed counterclockwise rotation, while previous studies report clockwise rotation of bore fronts at northern midlatitudes (Li et al., 2013; Smith et al., 2003). As event no. 2, we report a mesospheric bore with a very long wave front exceeding 2200 km. With the benefit of VISI's wide FOV, a new feature of the horizontally undulating wave front was captured. The vertical undulations following bore fronts have often been discussed since Dewan and Picard (1998) explained the subsequent undulation with vertical displacement in varicose mode. However, the horizontal undulation of mesospheric bore fronts has never been reported as far as we know. This paper is the first report of an undulating bore front.

2 Instrumentation and methodology

VISI is a visible and near-infrared spectral imager that was installed on the ISS, and made observations from September 2012 to August 2015. VISI has a grism as a disperser, and the spectral resolution (λ∕Δλ) is ∼ 800. The detector is a back-illuminated, frame transfer CCD (e2V 47-20 AIMO), with 1024 × 1024 pixel format, 13 × 13 µm single pixel size, and 0.92 of quantum efficiency at 630 nm. The column axis of CCD is for space, and the raw axis is for wavelength. On-chip binning is performed along the column (spatial) axis with a nominal binning size of 16 pixel. It has two slit-shaped FOVs that are perpendicular to the ISS orbit track and 45^∘ forward/backward to nadir. VISI performs continuous line-scan imaging and provides seamless two-dimensional images of airglows. The nominal exposure time is 1.0 s. Since it requires 0.9 s reading time, the exposure cycle is 1.9 s. The main targets of VISI are O₂ (0–0) at 762 nm, OH Meinel at 730 nm, and OI at 630 nm. In the nominal operation, the peak (maximum) and background (minimum) counts in the wavelength range around the center (762, 730 or 630 nm) ± 6 nm are recorded. By subtracting the background count from the peak count, and multiplying the calibration factor, the airglow intensity is obtained. See Sakanoi et al. (2011) for more details on the instrumentation.

Data of O₂ (0–0) airglow at 762 nm were utilized in this study. Because there is strong absorption by the ground-state O₂ in the lower atmosphere, the O₂ (0–0) band is not sensitive to contamination from lower altitudes, such as city lights or moon light refraction from the cloud top. The nominal altitude of the emission is 95 km, so data were mapped to the altitude of 95 km. Assuming an ellipsoid with the eccentricity of World Geodetic System 84 (WGS84) and an equatorial axis of wgs84A (6378.137 km) + 95 km as the altitude plane of 95 km, the intersection point between the ellipsoid surface and the line of sight of each pixel was calculated. Then, we mapped the airglow intensity to the intersection point, and obtained the two-dimensional airglow image. At the mapping altitude, the horizontal width of FOV is 670 km. The spatial resolutions are 13 km along and 12–15 km across the ISS orbit track. The typical phase speed of mesospheric bores is in the range of 60–80 m s⁻¹ (Bageston et al., 2011; Fechine et al., 2009; Giongo et al., 2018; Li et al., 2013; Medeiros et al., 2001; Narayanan et al., 2009; Nielsen et al., 2006; She et al., 2004; Smith et al., 2003, 2005; Taylor et al., 1995). To the best of our knowledge, the highest bore phase speeds reported in the literature are 98±8 m s⁻¹ (Brown et al., 2004). The speed of the ISS is 7.4 km s⁻¹, which is significantly higher than the typical phase speed of mesospheric bores. Therefore, it is reasonable to consider that VISI observes snapshots of bore-induced airglow structure.

Temperature profiles obtained by the Sounding of the Atmosphere using Broadband Emission Radiometry (SABER) instrument onboard the Thermosphere, Ionosphere, Mesosphere, Energetics and Dynamics (TIMED) satellite were employed as supporting data to assess the background thermal structure. Vertical profiles of kinetic temperature can be retrieved from SABER measurements of CO₂ 1.5 µm earth limb emission (Mertens et al., 2001). The v2.0 level 2A data downloaded from http://saber.gats-inc.com (last access: 14 November 2018) were used in this study. The square Brunt–Väisälä frequency can be derived from a temperature profile as

$$\begin{array}{}\text{(2)}& {\displaystyle }{N}^{\mathrm{2}}={\displaystyle \frac{g}{T}}\left(\mathrm{\Delta }{T}_z+{\displaystyle \frac{g}{C_{\mathrm{p}}}}\right),\end{array}$$

where T is the temperature, ΔT_z is the vertical temperature gradient, and C_p is the specific heat at constant pressure. The square Brunt–Väisälä frequency at an altitude of z is obtained from two continuous SABER temperature data by substituting $T=\left(T\right(z_{\mathrm{1}})+T(z_{\mathrm{2}}\left)\right)/\mathrm{2}$ and $\mathrm{\Delta }{T}_z=\left(T\right(z_{\mathrm{2}})-T(z_{\mathrm{2}}\left)\right)/(z_{\mathrm{2}}-z_{\mathrm{1}})$ into Eq. (2) where $z=(z_{\mathrm{1}}+z_{\mathrm{2}})/\mathrm{2}$. The height step of the SABER data around 95 km is ∼ 0.4 km.

3 Results and discussion

3.1 Event no. 1

Figure 1 O₂ (762 nm) airglow images obtained by VISI with the forward and backward FOVs in two consecutive passes on 9 July 2015. Airglow images were mapped to the altitude of 95 km. Panels (a) and (b) show the mesospheric bore observed by the forward FOV in the first pass and second pass, respectively. The FOV crossed the front at 19:11:13 and 20:49:13 UT. Panels (c) and (d) show the mesospheric bore observed by the backward FOV in the first pass and second pass, respectively. The FOV crossed the front at 19:12:52 and 20:50:52 UT. Panels (e) and (f) show the airglow images obtained in the two passes are shown in one plot. The airglow data are the same as the above four plots, but the images are zoomed in to show detailed wave characteristics. Blue lines indicate the bore front and the wave crests.

A sharp front followed by undulations was observed by VISI on 9 July 2015 over the South Atlantic Ocean. The front was captured in two consecutive passes so that the temporal evolution of the structure can be investigated from the observations. The airglow images obtained by the forward and backward FOVs of VISI are shown in Fig. 1. In the first pass, the center of the forward and backward FOVs crossed the front at 19:11:13 and 19:12:52 UT. In the second pass, they crossed it again at 20:49:13 and 20:50:52 UT, respectively.

In the first observations (Fig. 1a, d), a sharp brightness jump of airglow followed by wave structures can be seen around 10^∘ E longitude with S–N elongation of the front. The western (eastern) side of the front is bright (dark), and the boundary is fine. We can see small wave trains whose wave fronts are parallel to the front of the brightness jump on the western side. The front and wave crests identified in VISI images are indicated with blue lines in Fig. 1e, f. The morphological feature is exactly the same as bore-induced airglow structures reported by previous studies. Since the undulations are seen on the western side of the front, the mesospheric bore is expected to propagate eastward. Two crests were identified on the southern part of the western side of the front. The interval of the crests is ∼30 km. Then, the wavelength of following waves is ∼30 km. The O₂ airglow brightness on the western side of the front is 2500–3000 R, which is 250 %–300 % brighter than that on the eastern side. Another enhancement of airglow brightness can be seen at 15–18^∘ E, but the boundary of this enhancement is not sharp, and we will not focus on this enhancement in this study.

In the second observations (Fig. 1b, d), the front moved eastward, and was observed at 16–25^∘ E. The amplitude of the brightness jump is almost the same as that in the first pass, 3000–3500 R in the western (bright) side as compared to 1300 R in the eastern (dark) side. The airglow intensities both sides of the wave front were slightly brighter than the intensities in the previous pass. At 50^∘ S, the front moved 620 km eastward in the interval. Thus, if we assume a pure eastward propagation, the bore speed is estimated as 100 m s⁻¹. This value is close to the bore speeds reported by previous studies that are typically 60–80 m s⁻¹. The undulations were identified on the southern part in the second pass as well as in the first pass. As shown in the Fig. 1e, f, the number of wave crests increased to seven in the second pass from two in the first pass. It means that the wave adding rate is expected to be 3.5 waves h⁻¹. This value is also similar to the wave adding rates reported previously that ranged from 1.3 to 8.6 waves h⁻¹ (Li et al., 2013; Narayanan et al., 2009; Nielsen et al., 2006; She et al., 2004; Smith et al., 2003, 2017; Taylor et al., 1995).

Figure 2 SABER measurements obtained 2.3 h after the bore event no. 1. (a) The measurement point at 95 km altitude is indicated by the black cross. (b) The altitude profile of temperature showing a 30 K temperature inversion at 95–100 km altitude. (c) The altitude profile of the resulting Brunt–Väisälä frequency showing a stable layer at 95–100 km.

Mesospheric bores are thought to require a channel or region of increased stability in which a bore propagates (Dewan and Picard, 1998). A mesospheric inversion layer, a large wind shear, or the combination of both can make such a structure. To assess the background condition of this bore event, both temperature and wind data are ideally needed. For the current case, however, wind data from radar or lidar are not available. Thus, we examine only background temperature structure with TIMED/SABER data. TIMED/SABER made a near-coincident observation (orbit 73617, event 82) 2.3 h after the second observation of VISI, at 23:10 UT on 9 July 2015, at 52.1^∘ S, 24.8^∘ E for 95 km altitude (Fig. 2a). Figure 2b presents the vertical temperature profile showing a 30 K temperature inversion at 95–100 km altitude, and a 10 K temperature inversion at 91–93 km. The vertical profile of Brunt–Väisälä frequency derived from SABER temperature measurement is presented in Fig. 2c. A stable layer, the region of strong stability (high N²) surrounded by low-stability or unstable regions (low or negative N²), is recognized at 95–100 km altitude. This is a favorable structure for mesospheric bores in which a bore propagates in varicose mode. An unstable region around 95 km appears narrow, while an unstable region at 90–91 km is relatively thick. Then, the lower limit of the stable region might be 91 km. In any case, TIMED/SABER data show the existence of a stable layer near the typical emission peak altitude (95 km) of 762 nm O₂ emission. Since temperature inversions are thought to be long-lived phenomena (Meriwether and Gardner, 2000; Meriwether and Gerrard, 2004), the stable layer due to the inversion layer observed by SABER is expected to exist during the VISI observation, 2.3 h before the SABER observation. The mesospheric bore is likely to propagate in the stable layer created by a temperature inversion.

The orientation of the wave front was a NNW–SSE direction in the second pass, while it was almost a N–S direction in the first pass. The azimuthal angle of the wave front was observed to rotate counterclockwise from 12^∘ (angle from north to east) to −18^∘ within one orbital period of the ISS. Thus, the rotation speed is −20^∘ h⁻¹. The difference of the phase speed of the front in the southern side and northern side might be a cause of the rotation. According to Eq. (1), the propagating speed of the bore depends on the depth of the ducting layer ($U\propto \sqrt{\mathrm{duct}\mathrm{depth}}$) and surrounding temperature structure (via g^′). If the layer depth is thicker on the southern side, the phase speed is larger there; then, the front rotates counter clockwise.

Figure 3 O₂ (762 nm) airglow images obtained by VISI with the forward and backward FOV on 7 May 2013. The start and end times of capturing the bore front are indicated with dashed lines.

The background wind is another important factor when we consider the rotation of the front. Generally, wind in the mesopause region is largely dominated by atmospheric tides and inertia gravity waves, and the majority of those are thought to propagate from lower atmosphere (Aso and Vincent, 1982; Nakamura et al., 1993). In winter midlatitudes, the semi-diurnal and diurnal tides have significant amplitude (Aso and Vincent, 1982). Upward propagating tides and waves have clockwise variations in the Northern Hemisphere and counterclockwise variations in the Southern Hemisphere due to the Coriolis acceleration. While the current bore in the southern midlatitude showed counterclockwise rotation, northern midlatitude bores reported in previous studies showed clockwise rotation. Smith et al. (2003) reported 6^∘ h⁻¹ clockwise rotation of a bore front over North America. Li et al. (2013) reported 8^∘ h⁻¹ clockwise rotation over northern China.

Figure 4 SABER measurements obtained from 7 May at 22:31 UT to 8 May at 01:43 UT. (a) The measurement points at 95 km are indicated by crosses. (b) The altitude profiles of temperature. (c) The altitude profiles of Brunt–Väisälä frequency.

Rotation directions of these bores in both the Northern and Southern Hemisphere are consistent with the expected background wind variations that were dominated by upward propagating tides and waves. The rotation of wave fronts might be caused by background wind variations. In the past studies, to the best of our knowledge, there was no report of mesospheric bores at southern midlatitudes, where the ground-based observation sites are not dense. VISI can provide the southern midlatitude data and show the hemispheric difference clearly.

The bore parameters, such as phase speed, wavelength of trailing waves, and wave adding rate, were similar to those reported by previous studies based on ground-based measurements. These similarities support the validity of VISI observation for mesospheric bores. Next, we will report on the large-scale spatial structure of a mesospheric bore revealed by the wide FOV of VISI.

Figure 5 (a) Possible interpretation of the undulating wave front. (b) Schematic picture of a proposed modulating duct structure.

3.2 Event no. 2

A mesospheric bore with a very long wave front was observed on 7 May 2013 over the South Atlantic Ocean (35–43^∘ S, 24^∘ W–1^∘ E) as shown in Fig. 3. A front, characterized by a sharp increase in brightness, elongated W to NW and E to SE was captured from 20:55:01 to 20:59:57 UT with the forward FOV, and from 20:55:51 to 21:01:26 UT with the backward FOV. The O₂ airglow brightness on the SSW side of the front is 4200–5000 R, that is 130 %–160 % brighter than that on the NNE side. Within the VISI's FOV, the wave front has a large horizontal extent exceeding 2200 km. The small wavy structures parallel to the wave front are seen at 8–0^∘ W on the SSW (bright) side of the wave front; thus, the bright front is expected to propagate NNE-ward. The wavelength of trailing waves is 50 km. An interesting feature of this event is the undulating wave front. The wave front of the bright jump was not straight. It undulated with a wavelength of ∼1000 km. The crests of the modulation are at 18^∘ W, 27^∘ S and 6^∘ W, 40^∘ S, where the front advanced forward to the propagating direction (NNE) compared to other portions of the front.

The same as event no. 1, there are no available wind data for this event. We only examine background temperature structure with TIMED/SABER data. Figure 4 shows the result of SABER measurement 1.5–4.5 h after the VISI observation. Since the horizontal extent of the bore front is zonally long, temperature data from three passes are presented.

The nearest measurement to the bore front was made at 25^∘ E, 40^∘ S for 95 km altitude at 23:10 UT on 7 May 2013 (orbit 61836, event 57, blue line). In the temperature profile, a large 60 K temperature inversion layer is recognized at 93–100 km altitude. Figure 2c indicates the existence of a corresponding stable layer at 93–97 km favorable for mesospheric bore propagation. In the temperature profile of the previous pass (orbit 61835, event 58, red line), a temperature inversion can be seen at a similar altitude (93–95 km), but the intensity of inversion is much smaller. It is less than 30 K. The temperature profile of the following pass (orbit 61837, event 55, green line) shows temperature inversions at 89–93 km and 100–105 km; they are a little lower and higher than the previous two passes. Since three temperature profiles show the existence of a temperature inversion layer near the emission height, the mesospheric bore of event no. 2 seems to have propagated in the stable layer created by temperature inversion, the same as event no. 1.

In this event, VISI captured the very large spatial extent of a mesospheric bore exceeding 2200 km long. The result indicates that the propagating region due to a mesospheric inversion layer has a similar or larger spatial extent. Although the three SABER temperature profiles obtained with a 1000 km interval in the horizontal and a 1.5 h time interval show small discrepancies in the inversion amplitude and layer altitude, the stable layer caused by the inversion layer is expected to have one continuous large horizontal extension at the time when the bore propagated. Smith et al. (2003) reported a mesospheric bore propagating over 1000 km and a concurrent measurement of an inversion layer at a separate observation site, and showed that inversion layers with horizontal-scale sizes of 1000–1500 km can exist. Suzuki et al. (2013) demonstrated that a ducting gravity wave can propagate over 1800 km at mesopause height by using a network of ground-based imagers. These previous studies showed the horizontal extents of a propagating or ducting medium along the propagating direction of waves. Our result shows that the horizontal extents can also be large perpendicular to the propagating direction as it exceeds 2200 km.

While a curved or bent wave front of a mesospheric bore has been reported (Brown et al., 2004; Smith et al., 2017), to the best of our knowledge, an undulating wave front of a mesospheric bore has never been reported. The undulating wave front seen in Fig. 3 is a new feature of mesospheric bores that was revealed by the wide FOV of space-borne imaging. A possible explanation of the undulated wave front is nonuniform bore speed along the wave front. As illustrated in Fig. 5a, periodically modulating propagating speed can cause an undulating wave front. As mentioned above, the propagating speed of bore front depends on the depth of the ducting layer and surrounding temperature structure. A spatial inhomogeneity in the ducting structure, such as duct depth or thermal structure, can cause an inhomogeneity of bore speed in space. Figure 5b shows a schematic picture of the possible modulating duct structure. Since bore speed is proportional to the square root of duct depth, a larger bore speed is expected where the duct depth is large, and a smaller bore speed is expected where the duct depth is small. Thus, if there is a modulating duct as shown in Fig. 5b, it can yield nonuniform bore speed and a resultant modulating wave front. The bore front modulation in Fig. 3 shows a sinusoidal shape. It implies that the spatial inhomogeneity in the duct depth or temperature gradient also has sinusoidal modulation. This fact suggests that the modulation in the duct depth or temperature gradient might be a result of the interaction between the stable layer and a wave with horizontal wavelength of 1000 km.

A point-like tropospheric source location of an atmospheric gravity wave can be found by estimating the curvature of the observed wave front from airglow imagery with the assumption that the disturbance propagates radially from its source (Suzuki et al., 2007). An implication from the discussion of the undulated wave front is that such a method for source identification using the curvature of the wave front would be misleading in the case that the bore speed is nonuniform.

4 Summary

Two mesospheric bore events at southern midlatitudes observed by VISI were reported. For event no. 1, the temporal evolution of the bore was estimated from two consecutive VISI observations. Estimated bore parameters, such as phase speed, wavelength of trailing waves, and wave adding rate, were consistent with previous studies. These results validate the use of VISI for bore studies. This event provided information on the temporal evolution of the azimuth angle of the bore front in the southern midlatitudes. The bore was rotated counterclockwise with a speed of 20^∘ h⁻¹, while past studies reported clockwise rotating bores in the northern midlatitudes. The rotating directions are consistent with upward propagating tides and gravity waves, suggesting that the bore was affected by tidal backward wind variation. From event no. 2, with the benefit of the wide FOV of VISI, we found that (1) a wave front of a mesospheric bore can be long as it exceeds 2200 km, and (2) a wave front of a mesospheric bore is not always straight or simply curved in a large-scale view; it can periodically undulate. The undulating wave front of the bore suggests that the bore speed in the duct is not uniform in space. The space-borne imaging has a wide FOV and global observation coverage, and it can be utilized to study mesospheric bores at the synoptic scale. As a future work, we plan to conduct a statistical study on the global characteristics of mesospheric bores with VISI data.