Space Weather: The Solar Perspective

By R. Schwenn. 2006

496 citations recorded by the source corpus.

The term space weather refers to conditions on the Sun and in the solar wind, magnetosphere, ionosphere, and thermosphere that can influence the performance and reliability of space-borne and ground-based technological systems and that can affect human life and health. Our modern hi-tech society has become increasingly vulnerable to disturbances from outside the Earth system, in particular to those initiated by explosive events on the Sun: Flares release flashes of radiation that can heat up the terrestrial atmosphere such that satellites are slowed down and drop into lower orbits, solar energetic particles accelerated to near-relativistic energies may endanger astronauts traveling through interplanetary space, and coronal mass ejections are gigantic clouds of ionized gas ejected into interplanetary space that after a few hours or days may hit the Earth and cause geomagnetic storms. In this review, I describe the several chains of actions originating in our parent star, the Sun, that affect Earth, with particular attention to the solar phenomena and the subsequent effects in interplanetary space.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/83a83a7bbd85bd2db9e04ff499f4fd388afd4815

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In Astronomy and Astrophysics

1. M. Temmer
2. Nat Gopalswamy
3. T. Howard
4. N. Lugaz
5. D. Webb
6. A. Vourlidas
7. R. Howard
8. Yuming Wang

Citations in the corpus

• Coronal Mass Ejections: Observations (2012, background): “In addition, see also the Living Reviews by Schwenn (2006) and Chen (2011), and other Living Reviews in Solar Physics articles on prominences, flares, space weather, and other related phenomena.”
• Space Weather: Terrestrial Perspective (2007, background): “The interplanetary structure formed by the coronal mass ejection (ICME) propagates outward from the Sun, often at high velocity (Schwenn, 2006).”
• History and development of coronal mass ejections as a key player in solar terrestrial relationship (2016, background): “Excellent reviews on CMEs and the related phenomena already exist (Schwenn 2006; Chen 2011; Akasofu 2011; Webb and Howard 2012), so I focus only on the key milestones that led to the current understanding of CMEs.”
• The Heliospheric Magnetic Field (2013, background): “ICMEs produce the largest deviations from the Parker spiral magnetic field and are the primary source of strong meridional HMF in the nearEarth solar wind, making ICMEs particularly geoeffective (e.g., Gosling, 1993; Schwenn, 2006, and references therein).”
• The Interaction of Successive Coronal Mass Ejections: A Review (2016, background): “…are thought to be injected onto field lines located in the western SOLA: Review_v4.tex; 16 March 2017; 5:40; p. 13 hemisphere of the Sun, accounting for Sun-Earth connecting magnetic structures due to the Parker spiral shape of the IP magnetic field (see, e.g., Klein et al., 2008, Schwenn, 2006).”
• Solar Influence on Global and Regional Climates (2012, background): “Solar energetic particles (SEP) are emitted by solar flares and from the shock fronts that form ahead of super-sonic (and super-Alfve´nic) ejections of material from the corona (Schwenn 2006).”
• DIFFERENTIAL EMISSION MEASURE ANALYSIS OF MULTIPLE STRUCTURAL COMPONENTS OF CORONAL MASS EJECTIONS IN THE INNER CORONA (2012, background): “…corona (e.g., 3–10 R⊙), densities in the LFs are usually in the order of 104 to 106 cm−3, which represent ∼10–100 times enhancement over the background corona Electronic address: xincheng@nju.edu.cn Electronic address: jzhang7@gmu.edu at those heights (Ciaravella et al. 2003, 2005; Schwenn 2006).”
• Space weather: the solar perspective (2021, background): “From the historical perspective, the so-called ‘‘Carrington-event’’ from September 1, 1859 is the reference event for referring to extreme Space Weather and with that the beginning of Space Weather research (see also Schwenn 2006).”
• How Many CMEs Have Flux Ropes? Deciphering the Signatures of Shocks, Flux Ropes, and Prominences in Coronagraph Observations of CMEs (2012, background): “Our discussion suggests that it is time to rethink the original definition for a CME (Hundhausen et al., 1984), as expressed in Schwenn, 2006: “We define a CME to be an observable change in coronal structure that 1) occurs on a time scale of a few minutes and several hours and 2) involves the…”
• The magnetic field in the solar atmosphere (2014, background): “Here, we refer the interested reader to specialized reviews on the solar wind (Marsch, 2006; Ofman, 2010; Bruno and Carbone, 2013), space weather (Schwenn, 2006), and the heliospheric magnetic field (Owens and Forsyth,”
• Interplanetary conditions causing intense geomagnetic storms (Dst ≤ −100 nT) during solar cycle 23 (1996–2006) (2008, methodology): “A CME viewed near the sun has 3 fundamental components: the bright outer loops, a dark region and a filament [Hundhausen et al., 1984; Schwenn, 2006].”
• Origins of the Ambient Solar Wind: Implications for Space Weather (2017, background): “Table 1 summarizes some representative properties of the fast and slow wind regimes as revealed over the past half-century of exploration (see also Schwenn 2006).”