Astrophysics in 2006

Trimble, Virginia; Aschwanden, Markus J.; Hansen, Carl J.

doi:10.1007/s11214-007-9224-0

Cited by 12 publications

(8 citation statements)

References 2,049 publications

(1,289 reference statements)

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“…In addition to these four instrument teams, there are several groups devoted to global modeling (see Aschwanden et al 2007) with the goal of understanding the connection between the solar activity observed near the sun by SECCHI and S/WAVES and the in situ measurements taken by IMPACT, PLASTIC and S/WAVES when the disturbances finally reach the STEREO spacecraft. Modeling includes the coronal plasma and the solar wind and its expansion outwards from the Sun.…”

Section: • Stereo/waves (S/waves) Was Built By a Team Led By Jean-loumentioning

confidence: 99%

The STEREO Mission: An Introduction

et al. 2007

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The twin STEREO spacecraft were launched on October 26, 2006, at 00:52 UT from Kennedy Space Center aboard a Delta 7925 launch vehicle. After a series of highly eccentric Earth orbits with apogees beyond the moon, each spacecraft used close flybys of the moon to escape into orbits about the Sun near 1 AU. Once in heliospheric orbit, one spacecraft trails Earth while the other leads. As viewed from the Sun, the two spacecraft separate at approximately 44 to 45 degrees per year. The purposes of the STEREO Mission are to understand the causes and mechanisms of coronal mass ejection (CME) initiation and to follow the propagation of CMEs through the inner heliosphere to Earth. Researchers will use STEREO measurements to study the mechanisms and sites of energetic particle acceleration and to develop three-dimensional (3-D) time-dependent models of the magnetic topology, temperature, density and velocity of the solar wind between the Sun and Earth. To accomplish these goals, each STEREO spacecraft is equipped with an almost identical set of optical, radio and in situ particles and fields instruments provided by U.S. and European investigators. The SECCHI suite of instruments includes two white light coronagraphs, an extreme ultraviolet imager and two heliospheric white light imagers which track CMEs out to 1 AU. The IMPACT suite of instruments measures in situ solar wind electrons, energetic electrons, protons and heavier ions. IMPACT also includes a magnetometer to measure the in situ magnetic field strength and direction. The PLASTIC instrument measures the composition of heavy ions in the ambient plasma as well as protons and alpha particles. The S/WAVES instrument uses radio waves to track the location of CME-driven shocks and the 3-D topology of open field lines along which flow particles produced by solar flares. Each of the four instrument packages produce a small real-time stream of selected data for purposes of predicting space weather events at Earth. NOAA forecasters at the Space Environment

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Section: • Stereo/waves (S/waves) Was Built By a Team Led By Jean-loumentioning

confidence: 99%

The STEREO Mission: An Introduction

et al. 2007

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“…Kurtz, Eichhorn, Accomazzi, Grant, Demleitner, Murray, and colleagues (2005) pointed out that the series of papers by Trimble and colleagues: “Astrophysics in XXXX” (where XXXX is the immediate past year) each year is routinely the most used paper in astronomy, but is very rarely cited; for example, the most recent two, (Trimble, Aschwanden, & Hansen, 2006, 2007) have yet to be cited (as this is written). These papers are like newspapers in their usefulness.…”

Section: Usage Bibliometricsmentioning

confidence: 99%

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Kurtz

Bollen

2010

Annual Review Info Sci & Tec

122

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“…However, in the Hubble flow the space itself expands with no centre. In a PN, there is a well‐defined centre of the expanding gas; see Trimble, Aschwanden & Hansen 2007. )…”

Section: Introductionmentioning

confidence: 99%

Shaping planetary nebulae by light jets

Akashi¹,

Soker²

2008

Monthly Notices of the Royal Astronomical Society

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We conduct numerical simulations of axisymmetrical jets expanding into a spherical asymptotic giant branch (AGB) slow wind. The three-dimensional flow is simulated with an axially symmetric numerical code. We concentrate on jets that are active for a relatively short time. Our results strengthen other studies that show that jets can account for many morphological features observed in planetary nebulae (PNs). Our main results are as follows. (1) With a single jet's launching episode, we can reproduce a lobe structure having a 'front lobe', that is a small bulge on the front of the main lobe, such as that in the PN Mz 3. (2) In some runs, dense clumps are formed along the symmetry axis, such as those observed in the pre-PN M1-92. (3) The mass-loss history of the slow wind has a profound influence on the PN structure. (4) A dense expanding torus (ring; disc) is formed in most of our runs. The torus is formed from the inflated lobes and not from a separate equatorial mass-loss episode. (5) The torus and lobes are formed at the same time and from the same mass-loss rate episode. However, when the slow wind density is steep enough, the ratio of the distance divided by the radial velocity is larger for regions closer to the equatorial plane than for regions closer to the symmetry axis. (6) With the short jet-active phase, a linear relation between distance and expansion velocity is obtained in many cases. (7) Regions at the front of the lobe are moving sufficiently fast to excite some visible emission lines.

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Astrophysics in 2006

Cited by 12 publications

References 2,049 publications

The STEREO Mission: An Introduction

The STEREO Mission: An Introduction

Usage bibliometrics

Shaping planetary nebulae by light jets

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