Next Article in Journal
Homogenization of the Probability Distribution of Climatic Time Series: A Novel Algorithm
Previous Article in Journal
Influence of Building-Height Variability on Urban Ventilation and Pollutant Dispersion Characteristics
Previous Article in Special Issue
Deep Learning-Based Vertical Decomposition of Ionospheric TEC into Layered Electron Density Profiles
 
 
Search for Articles:
Title / Keyword
Author / Affiliation / Email
Journal
Article Type
 
 
Advanced Search
 
Section
Special Issue
Volume
Issue
Number
Page
 
Journals
Atmosphere
Volume 16
Issue 5
10.3390/atmos16050615
atmosphere-logo
Submit to this Journal Review for this Journal Propose a Special Issue
► Article Menu

Article Menu

share Share announcement Help format_quote Cite
first_page
settings
Order Article Reprints
Font Type:
Arial Georgia Verdana
Font Size:
Aa Aa Aa
Line Spacing:
Column Width:
Background:
Article

A Forgotten Aurora: Revisiting the 19 March 1950 Aurora Australis Through Historical Records

by
Víctor M. S. Carrasco
1 and
José M. Vaquero
2,*
1
Departamento de Física, Universidad de Extremadura, 06006 Badajoz, Spain
2
Instituto Universitario de Investigación del Agua, Cambio Climático y Sostenibilidad (IACYS), Universidad de Extremadura, 06006 Badajoz, Spain
*
Author to whom correspondence should be addressed.
Atmosphere 2025, 16(5), 615; https://doi.org/10.3390/atmos16050615 (registering DOI)
Submission received: 17 April 2025 / Revised: 3 May 2025 / Accepted: 15 May 2025 / Published: 18 May 2025
(This article belongs to the Special Issue Research and Space-Based Exploration on Space Plasma)
Browse Figures
Versions Notes

Abstract

:
This study investigates the aurora australis event of 19 March 1950, which was reported across multiple locations in Australia, including Hobart, Sydney, and as far north as Goondiwindi. Despite its significance as a historical space weather event, this aurora has received little attention in the scientific literature. Using contemporary news reports from The Sydney Morning Herald and Mercury, we reconstruct the characteristics of the event. Observers described vivid red and green auroral displays with streamers, indicative of intense geomagnetic activity. The associated geomagnetic storm reached a Kp index of 7+. We have estimated the magnetic disturbance peak of −278 nT (±15 nT) from measurements made in the Kakioka Magnetic Observatory. This would place it among the top 50 most intense storms recorded since 1957, according to the Dst index, though still significantly below the most extreme events. Notably, this aurora is absent from modern auroral catalogs, and no documented observations from the Northern Hemisphere have been identified. These findings underscore the critical role of historical records in advancing our understanding of auroral phenomena and their relationship with solar activity. Given the provisional nature of this study, further historical documents may yet emerge, providing additional insights into this event and its broader space weather context.

1. Introduction

Solar activity manifests in several phenomena, including, for example, sunspots, solar flares, and coronal mass ejections [1]. These solar phenomena can release immense amounts of energy into space, interacting with Earth’s magnetosphere to produce auroras [2,3,4]. While auroras are often confined to high latitudes, significant geomagnetic storms can expand their visibility to mid- or even low-latitude regions [5,6,7].
Historical records of auroras are valuable proxies to know past solar activity [8,9]. Aurora data provide complementary information to other indices of solar activity [10,11]. These events, documented in diverse sources such as newspapers, personal diaries, and scientific observations, show patterns of solar variability over centuries [12,13]. For example, newspapers became key documentary sources for such reports in the 19th and 20th centuries [14]. However, some auroral events in the Southern Hemisphere remain underrepresented in modern catalogs, emphasizing the importance of revisiting and analyzing historical records to enrich our understanding of auroral and past solar activity. This is the case of the great aurora on 19 March 1950.
This study focuses on one overlooked event, the aurora australis of 19 March 1950, providing a detailed analysis based on Australian newspaper reports and geomagnetic data. We show two news articles including information on this event in Section 2. An analysis of these articles is made in Section 3. Section 4 includes information on solar activity to contextualize the geomagnetic storm. An estimation of the magnetic disturbance of the storm is shown in Section 5. The main conclusions of this work are in Section 6.

2. Documentary Sources

The sources of the aurora event presented in this work are news items published in the Australian newspapers The Sydney Morning Herald (from Sydney, New South Wales) and the Mercury (from Hobart, Tasmania). These newspapers were important documentary sources publishing information on natural phenomena and scientific news items in mid-20th century Australia. Note that newspapers were a key means of disseminating information about unusual occurrences such as auroras.
A digital archive of these newspapers is maintained in the Trove database (https://trove.nla.gov.au/, accessed on 17 April 2025), a collaboration between the National Library of Australia and hundreds of partner organizations around Australia. Trove facilitates the preservation and accessibility of historical documents, enabling modern researchers to find details of past events such as the aurora australis of 19 March 1950. Two news articles, including information on the visibility, timing, and characteristics of the aurora australis seen on 19 March 1950, published in the aforementioned newspapers, can be found in Figure 1.

3. Analysis of the Aurora Reports

The auroral oval in the Southern Hemisphere typically lies around 65° magnetic latitude during periods of low geomagnetic activity. During strong geomagnetic storms classified as G3 or greater on the NOAA scale, the oval can expand significantly toward lower latitudes, sometimes reaching as low as ~40° magnetic latitude or below [15].
The reports analyzed in this work describe a brilliant auroral display visible in several regions across Australia. Records were confirmed in Hobart (42.9° S and magnetic latitude of 51.5° S), Sydney (34.5° S and magnetic latitude of 42.1° S), Ceduna (32.1° S and magnetic latitude of 42.5° S), and even as far north as in Goondiwindi (28.5° S and magnetic latitude of 37.0° S), an exceptional location to see auroras that show the reach of the event. The values provided for magnetic latitudes correspond to 1950. Changes in magnetic latitudes in the observation sites since 1950 are not significant. For example, the current magnetic latitude of Goondiwindi is 34.9° S, a change of just over 2°. The other observation sites show similar small variations. Therefore, the geomagnetic storm studied in this work can be compared to contemporary events in terms of latitudinal extent and geomagnetic context.
The aurora started at 7 p.m. in Hobart, reaching its peak at 9 p.m., whereas it was observed between 8:30 and 10:30 p.m. in Sydney. The aurora was seen with green and red lights with streamers extending across the sky. In particular, according to The Sidney Morning Herald, most of the observers described the aurora as a brilliant red glow. However, observers from Hobart reported a particularly vivid display of green sky with red streamers upwards, indicative of an intense geomagnetic field. An interesting information extracted from the observers from Hobart is that the aurora was almost overhead in that place: “[…] streamers of multi-coloured rays fanned out across the sky from the south-east to the north-west, converging to a point almost directly overhead”.
Despite its intensity, this aurora is not included in several modern auroral catalogs [13]. For example, no aurora records of this event in the Northern Hemisphere are included in Odenwald [14,16], who collected news items on geomagnetic storms and their impacts since the Carrington event. According to Odenwald [14,16], only two auroras in 1950 were reported in newspapers: those on 20 February and 19 August, the two most intense geomagnetic storms in 1950 according to the Kp index, as previously mentioned. News articles of these events were published in The New York Times on 21 February [17] and 20 August [18], indicating impacts such as disruptions in the radio cable service in the first case and a long blackout in the radio and press messages around the world.

4. Solar Activity Context

The aurora event presented in this work occurred during Solar Cycle 18. This cycle started in February 1944 and finished in March 1954. It was a strong cycle with a maximum value of 218.7 in May 1947 according to the 13-month smoothed sunspot number (https://www.sidc.be/SILSO, accessed on 17 April 2025). Note that the mean of the maximum amplitudes for Solar Cycles 1–24 according to the 13-month smoothed sunspot number is around 180. Therefore, this event occurred around the middle of the declining phase of Solar Cycle 18. The monthly sunspot number in March 1950 was 155.4. Sunspot drawings made in the Mount Wilson Observatory and Sacramento Peak Observatory are shown in Figure 2 [19,20]. Note that the east (west) side is in the right (left) part of the drawings. The number of groups recorded in those drawings was seven by the Mount Wilson Observatory and six groups in the Sacramento Peak Observatory. One group with a great sunspot was located around the central meridian of the Sun on that date, according to both drawings. A coronal mass ejection with origin in this active region could be responsible for the geomagnetic storm on 19 March 1950, causing the aurora australis.
The geomagnetic storm causing this aurora event is ranked in the 8th position of the most intense geomagnetic storms that occurred in 1950 according to the Kp index [21]. The maximum value of the Kp index reached during this storm was 7+ from 9–12 h to 15–18 h UTC on 19 March. Previously, the Kp index reached the value of 7- at 6–9 h UTC and decreased to 5 at 18–21 h UTC. Thus, this storm would be classified as G3 (strong) according to the current NOAA (National Oceanic and Atmospheric Administration) scale. The value of the Ap index for this event was 84, the fourth highest value that year. Note that the two most intense geomagnetic storms occurred on 20 February (Kp index value of 9-) and 19 August (Kp index value of 8+). However, although the February 1950 geomagnetic storm was stronger, the report from The Sidney Morning Herald pointed out that the last aurora seen before that in March 1950 was in May 1949, and the Mercury indicated that the aurora seen in March 1950 was the most brilliant, at least, in the two years before.
Despite the brightness and the behaviour of this aurora event on 19 March 1950, it is not in the top 50 of the strongest geomagnetic storms of Solar Cycle 18 according to the Kp index. Note that the two most intense geomagnetic storms of that cycle occurred on 22 September and 27 July 1646, both reaching a Kp index of 9. Data of the Kp and Ap index shown in this work were taken from the GFZ Postdam website (https://kp.gfz-potsdam.de, accessed on 17 April 2025).

5. Intensity of the 19 March 1950 Storm

We have estimated the values of the magnetic disturbance (in nT) for this geomagnetic storm using the data provided by the Kakioka Magnetic Observatory ([22], http://www.kakioka-jma.go.jp/en/, accessed on 17 April 2025) in Japan (36.2° N, 140.2° E). We note that the Dst index must be estimated from four near-equatorial observatories, but, unfortunately, we have not found data from other observatories for the date when this geomagnetic storm occurred. However, our results give a rough estimate of the Dst values reached during this storm.
The disturbance was obtained as [23]:
D(t) = H(t) − B − Sq(t)
where H is the observed value of the hourly H-component magnetic field, B is the baseline of H, and Sq is the solar quiet daily variations. We selected B as H hourly value of the pre-storm level at 1 h UTC on 19 March 1950. We selected five quiet days previous to the storm (26 February and 10–13 March) based on the revised daily Aa index by Lockwood et al. [24,25] to calculate the Sq variations. Then, it is divided by the cosine of its magnetic latitude (25.77° N). Figure 3 depicts the magnetic disturbance values estimated for the geomagnetic storm on 19 March 1950.
One can see that the magnetic disturbance values increased significantly from 1:00 h to 5:00 h UTC on 19 March 1950. Then, it sharply decreased until reaching a minimum value of −278 nT at 11:00 h UTC. Six hours later, the magnetic disturbance values were around −100 nT, and a relatively long recovery phase followed it. Considering the limitations of our approach, particularly the use of a single observatory, we estimate the uncertainty in the magnetic disturbance values to be approximately ±15 nT. This estimate takes into account the determination of B (±8 nT) and of Sq variations (±7 nT).
The estimated magnetic disturbance peak value for this storm would rank in the top 50 of the greatest geomagnetic storms according to the Dst index provided by the World Data Center for Geomagnetism in Kyoto (https://wdc.kugi.kyoto-u.ac.jp/, accessed on 17 April 2025) since 1957. However, the intensity of this storm is far from the strongest storms recorded since then such as those occurred in March 1989 (−589 nT) and July 1959 (−429 nT) [26], and others before 1957 as the Carrington storm and those occurred in 1872 and 1921 with minimum Dst values around −1000 nT [27,28,29].

6. Conclusions

This study has examined the aurora australis of 19 March 1950, a significant historical space weather event reported across Australia but, to date, unrecognized in the Northern Hemisphere. Despite its notable characteristics, this aurora has received little scientific attention. The visibility and reporting of auroras are not determined only by the intensity of the geomagnetic storm. Several factors must converge for an aurora to be observed and recorded, especially in regions where such phenomena are rare. These include the local time of the storm’s peak (auroras are only visible at night), favorable weather conditions (clear skies), and the level of public awareness or media interest at the time.
Using contemporary newspaper accounts, we have reconstructed its key features, including its vivid red and green displays, its remarkable visibility at mid-latitudes, and its association with an intense geomagnetic storm. The storm reached a Kp index of 7+, which would classify it as a G3 event on the modern NOAA scale. This case highlights that auroras observed at unusually low latitudes can be linked to geomagnetic storms that, while intense, do not necessarily fall into the extreme category.
We estimated the peak of the magnetic disturbance of this storm at −278 nT, using data from the Kakioka Magnetic Observatory (with an uncertainty of −15 nT). According to the Dst index, this storm would be in the top 50 of the strongest geomagnetic storms recorded since 1957. However, we acknowledge some limitations to this result. First, we note that we only found data from one observatory, and the Dst index must be calculated using data from four different observatories. Moreover, some historical geomagnetic storms show a significant asymmetry of the H-component measured in different observatories during the maximum phase of the events [30]. Then, the abrupt changes in the H-component observed in some observatories disappear in the average to calculate the Dst index in the case of asymmetry.
The event’s peak intensity coincided with nighttime hours at longitudes near Australia, while its intensity diminished as nightfall progressed across other regions. Given this, auroras should have been observable at similar longitudes in the Northern Hemisphere, such as in Japan and China. However, no documented observations from these locations have yet been identified. It remains plausible that Northern Hemisphere accounts of this event exist but have not yet been uncovered, underscoring the need for further investigation to refine our understanding of this geomagnetic storm.
Historical newspaper archives have proven to be valuable resources for reconstructing past auroral activity, particularly at low- and mid-latitudes where direct scientific observations may be scarce. They provide critical information for enhancing the historical record of auroras and improving our knowledge of past solar activity. Given the provisional nature of this study, future discoveries of additional historical records may offer further insights into this event and its broader implications for space weather research.

Author Contributions

Conceptualization, V.M.S.C.; methodology, V.M.S.C.; formal analysis, V.M.S.C.; writing—original draft preparation, V.M.S.C.; writing—review and editing, J.M.V.; project administration, J.M.V.; funding acquisition, J.M.V. All authors have read and agreed to the published version of the manuscript.

Funding

This research was funded by the Junta de Extremadura, grant no. GR24049.

Institutional Review Board Statement

Not applicable.

Informed Consent Statement

Not applicable.

Data Availability Statement

No new data was created in this work.

Acknowledgments

The authors acknowledge the National Library of Australia for providing the newspapers consulted in this work. We also acknowledge the GFZ Potsdam for hosting geomagnetic index data, the Kakioka Magnetic Observatory and SILSO for making geomagnetic field measurements available, and SILSO for providing sunspot number values. Additionally, we thank the institutions that maintain the solar observation archives at the Mount Wilson and Sacramento Peak Observatories.

Conflicts of Interest

The authors declare no conflicts of interest.

References

  1. Usoskin, I.G. A history of solar activity over millennia. Living Rev. Sol. Phys. 2023, 20, 2. [Google Scholar] [CrossRef]
  2. Akasofu, S.I. The Northern Lights: Secrets of the Aurora Borealis; Alaska Northwest Books: Portland, OR, USA, 2009. [Google Scholar]
  3. Vaquero, J.M.; Vázquez, M. The Sun Recorded Through History; Springer: Berlin, Germany, 2009. [Google Scholar]
  4. Cliver, E.W.; Schrijver, C.J.; Shibata, K.; Usoskin, I.G. Extreme solar events. Living Rev. Sol. Phys. 2022, 19, 1. [Google Scholar] [CrossRef]
  5. Silverman, S.; Cliver, E.W. Low-latitude auroras: The magnetic storm of 14–15 May 1921. J. Atmos. Sol.-Terr. Phys. 2001, 63, 523. [Google Scholar] [CrossRef]
  6. Knipp, D.J.; Ramsay, A.C.; Beard, E.D.; Boright, A.L.; Cade, W.B.; Hewins, I.M.; McFadden, R.H.; Denig, W.F.; Kilcommons, L.M.; Shea, M.A.; et al. The May 1967 great storm and radio disruption event: Extreme space weather and extraordinary responses. Space Weather 2016, 14, 614. [Google Scholar] [CrossRef]
  7. Hayakawa, H.; Hattori, K.; Pevtsov, A.A.; Ebihara, Y.; Shea, M.A.; McCracken, K.G.; Daglis, I.A.; Bhaskar, A.T.; Ribeiro, P.; Knipp, D.J. The Intensity and Evolution of the Extreme Solar and Geomagnetic Storms in 1938 January. ApJ 2021, 909, 2. [Google Scholar] [CrossRef]
  8. Eather, E.H. Majestic Lights; American Geophysical Union: Washington, DC, USA, 1980. [Google Scholar]
  9. Vaquero, J.M.; Trigo, R.M. Auroras in the Iberian Peninsula: Observations from 1700 to 1900. Solar Phys. 2005, 231, 157. [Google Scholar] [CrossRef]
  10. Eddy, J. The Maunder Minimum. Science 1976, 192, 1189–1202. [Google Scholar] [CrossRef]
  11. Silverman, S.M. Secular variation of the aurora for the past 500 years. Rev. Geophys. 1992, 30, 333. [Google Scholar] [CrossRef]
  12. Siscoe, G.L. Evidence in the auroral record for secular solar variability. Rev. Geophys. Space Phys. 1980, 18, 647. [Google Scholar] [CrossRef]
  13. Vázquez, M.; Vaquero, J.M.; Gallego, M.C.; Roca Cortés, T.; Pallé, P.L. Long-Term Trends and Gleissberg Cycles in Aurora Borealis Records (1600–2015). Solar Phys. 2016, 291, 613. [Google Scholar] [CrossRef]
  14. Odenwald, S. Newspaper reporting of space weather: End of a golden age. Space Weather 2007, 5, S11005. [Google Scholar] [CrossRef]
  15. Blake, S.P.; Pulkkinen, A.; Shuck, P.W.; Glocer, A.; Tóth, G. Estimating Maximum Extent of Auroral Equatorward Boundary Using Historical and Simulated Surface Magnetic Field Data. JGR Space Phys. 2021, 126, e2020JA028284. [Google Scholar] [CrossRef]
  16. Odenwald, S. The History of Space Weather. Independently Published. 2021. Available online: https://sten.astronomycafe.net (accessed on 17 April 2025).
  17. The New York Times. 21 February. Sun Storm Disrupts Cable, Radio Service, 1950. Available online: https://www.nytimes.com/1950/02/21/archives/sun-storm-disrupts-cable-radio-service.html?searchResultPosition=3 (accessed on 17 April 2025).
  18. The New York Times. 20 August. News from Korea Cut off for Hours, 1950. Available online: https://www.nytimes.com/1950/08/20/archives/news-from-korea-cut-off-for-hours-armys-taking-of-equipment.html?searchResultPosition=10 (accessed on 17 April 2025).
  19. Baranyi, T.; Győri, L.; Ludmány, A. On-line Tools for Solar Data Compiled at the Debrecen Observatory and their Extensions with the Greenwich Sunspot Data. Solar Phys. 2016, 291, 3081. [Google Scholar] [CrossRef]
  20. Carrasco, V.M.S.; Pevtsov, A.A.; Nogales, J.M.; Vaquero, J.M. The Sunspot Drawing Collection of the National Solar Observatory at Sacramento Peak (1947–2004). Solar Phys. 2021, 296, 3. [Google Scholar] [CrossRef]
  21. Bartels, J. The geomagnetic measures for the time-variations of solar corpuscular radiation, described for use in correlation studies in other geophysical fields. Ann. Intern. Geophys. 1957, 4, 209. [Google Scholar]
  22. Kakioka Magnetic Observatory. Kakioka Geomagnetic Field 1-h Digital Data in IAGA-2002 Format [Dataset]; Kakioka Magnetic Observatory Digital Data Service: Ishioka, Japan, 2013. [CrossRef]
  23. Sugiura, M. Hourly values of equatorial Dst for the IGY. Ann. Int. Geophys. Year 1964, 35, 9. [Google Scholar]
  24. Lockwood, M.; Chambodut, A.; Barnard, L.A.; Owens, M.J.; Clarke, E. A homogeneous aa index: 1. Secular variation. J. Space Weather Space Clim. 2018, 8, A53. [Google Scholar] [CrossRef]
  25. Lockwood, M.; Finch, I.D.; Chambodut, A.; Barnard, L.A.; Owens, M.J.; Clarke, E. A homogeneous aa index: 2. hemispheric asymmetries and the equinoctial variation. J. Space Weather Space Clim. 2018, 8, A58. [Google Scholar] [CrossRef]
  26. Boteler, D.H. A 21st Century View of the March 1989 Magnetic Storm. Space Weather 2019, 17, 1427. [Google Scholar] [CrossRef]
  27. Hayakawa, H.; Ebihara, Y.; Willis, D.M.; Toriumi, S.; Iju, T.; Hattori, K.; Wild, M.N.; Oliveira, D.M.; Ermolli, I.; Ribeiro, J.R.; et al. Temporal and Spatial Evolutions of a Large Sunspot Group and Great Auroral Storms Around the Carrington Event in 1859. Space Weather 2019, 17, 1553. [Google Scholar] [CrossRef]
  28. Hayakawa, H.; Cliver, E.W.; Clette, F.; Ebihara, Y.; Toriumi, S.; Ermolli, I.; Chatzistergos, T.; Hattori, K.; Knipp, D.J.; Blake, S.P.; et al. The Extreme Space Weather Event of 1872 February: Sunspots, Magnetic Disturbance, and Auroral Displays. ApJ 2023, 959, 23. [Google Scholar] [CrossRef]
  29. Love, J.J.; Hayakawa, H.; Cliver, E.W. Intensity and Impact of the New York Railroad Superstorm of May 1921. Space Weather 2019, 17, 1281. [Google Scholar] [CrossRef]
  30. Saiz, E.; Cid, C.; Gerrero, A. The relevance of local magnetic records when using extreme space weather events as benchmarks. J. Space Weather Space Clim. 2021, 11, 35. [Google Scholar] [CrossRef]
Atmosphere 16 00615 g001
Figure 1. News items published by The Sidney Morning Herald (left) and Mercury (right) on 20 March 1950 detailing the aurora australis observed the previous night [Source: https://trove.nla.gov.au, accessed on 17 April 2025].
Figure 1. News items published by The Sidney Morning Herald (left) and Mercury (right) on 20 March 1950 detailing the aurora australis observed the previous night [Source: https://trove.nla.gov.au, accessed on 17 April 2025].
Atmosphere 16 00615 g001
Atmosphere 16 00615 g002
Figure 2. Sunspot drawings recorded in the Mount Wilson Observatory (top panel) and Sacramento Peak Observatory (bottom panel) on 17 March 1950 [Sources: http://fenyi.solarobs.epss.hun-ren.hu/GPR/, accessed on 17 April 2025; https://www.ngdc.noaa.gov/stp/, accessed on 17 April 2025].
Figure 2. Sunspot drawings recorded in the Mount Wilson Observatory (top panel) and Sacramento Peak Observatory (bottom panel) on 17 March 1950 [Sources: http://fenyi.solarobs.epss.hun-ren.hu/GPR/, accessed on 17 April 2025; https://www.ngdc.noaa.gov/stp/, accessed on 17 April 2025].
Atmosphere 16 00615 g002
Atmosphere 16 00615 g003
Figure 3. Magnetic disturbance values (in nT) estimated from 16 March to 21 March 1950 using data from the Kakioka Magnetic Observatory.
Figure 3. Magnetic disturbance values (in nT) estimated from 16 March to 21 March 1950 using data from the Kakioka Magnetic Observatory.
Atmosphere 16 00615 g003
Disclaimer/Publisher’s Note: The statements, opinions and data contained in all publications are solely those of the individual author(s) and contributor(s) and not of MDPI and/or the editor(s). MDPI and/or the editor(s) disclaim responsibility for any injury to people or property resulting from any ideas, methods, instructions or products referred to in the content.

Share and Cite

MDPI and ACS Style

Carrasco, V.M.S.; Vaquero, J.M. A Forgotten Aurora: Revisiting the 19 March 1950 Aurora Australis Through Historical Records. Atmosphere 2025, 16, 615. https://doi.org/10.3390/atmos16050615

AMA Style

Carrasco VMS, Vaquero JM. A Forgotten Aurora: Revisiting the 19 March 1950 Aurora Australis Through Historical Records. Atmosphere. 2025; 16(5):615. https://doi.org/10.3390/atmos16050615

Chicago/Turabian Style

Carrasco, Víctor M. S., and José M. Vaquero. 2025. "A Forgotten Aurora: Revisiting the 19 March 1950 Aurora Australis Through Historical Records" Atmosphere 16, no. 5: 615. https://doi.org/10.3390/atmos16050615

APA Style

Carrasco, V. M. S., & Vaquero, J. M. (2025). A Forgotten Aurora: Revisiting the 19 March 1950 Aurora Australis Through Historical Records. Atmosphere, 16(5), 615. https://doi.org/10.3390/atmos16050615

Note that from the first issue of 2016, this journal uses article numbers instead of page numbers. See further details here.

Article Metrics

Article metric data becomes available approximately 24 hours after publication online.
Back to TopTop