Measurement of3He/4He in the Local Interstellar Medium: the Collisa Experiment onMir

Salerno, E.; Bühler, F.; Bochsler, P.; Busemann, H.; Bassi, M.; Zastenker, G. N.; Agafonov, Yu. N.; Éismont, N. A.

doi:10.1086/346203

Cited by 20 publications

(15 citation statements)

References 22 publications

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“…The ratios 22 Ne/ 20 Ne ∼ 0.073 and 18 O/ 16 O ∼ 0.002 are close to isotopic ratios in the solar wind (Cummings and Stone 2007;Leske 2000). He data gives 3 He/ 4 He ∼ 1.7 × 10 −4 , which is similar to meteoritic and HII region values (Salerno et al 2003;Gloeckler and Fisk 2007). Evidently the expected 3 He enrichment of the ISM by nucleosynthesis in low-mass stars has not affected the CHISM.…”

Section: Heliospheric Ismsupporting

confidence: 76%

“…Interstellar material (ISM) is observed at the Earth's orbit, where interstellar He 0 has been counted by the Ulysses GAS detector and is detected through fluorescence of solar 584 Å (Weller and Meier 1981;Flynn et al 1998;Salerno et al 2003;Witte 2004;Möbius et al 2004). Interstellar H 0 and other neutral interstellar atoms are driven into the heliosphere by the relative Sun-cloud motion of 26.2 km s −1 , where they become ionized and processed into pickup ions and anomalous cosmic rays.…”

Section: Introductionmentioning

confidence: 99%

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Is the Sun Embedded in a Typical Interstellar Cloud?

Frisch

2008

Space Sci Rev

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The physical properties and kinematics of the partially ionized interstellar material (ISM) near the Sun are typical of warm diffuse clouds in the solar vicinity. The direction of the interstellar magnetic field at the heliosphere, the polarization of light from nearby stars, and the kinematics of nearby clouds are naturally explained in terms of the S1 super-bubble shell. The interstellar radiation field at the Sun appears to be harder than the field ionizing ambient diffuse gas, which may be a consequence of the low opacity of the tiny cloud surrounding the heliosphere. The spatial context of the Local Bubble is consistent with our location in the Orion spur.

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Section: Heliospheric Ismsupporting

confidence: 76%

Section: Introductionmentioning

confidence: 99%

Is the Sun Embedded in a Typical Interstellar Cloud?

Frisch

2008

Space Sci Rev

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“…The ratios 22 Ne/ 20 Ne ∼ 0.073 and 18 O/ 16 O ∼ 0.002 are close to isotopic ratios in the solar wind [7,37]. He data gives 3 He/ 4 He ∼ 1.7 − 2.2 × 10 −4 , which is similar to meteoritic and HII region values [58,22]. Evidently the expected 3 He enrichment of the ISM by nucleosynthesis in low-mass stars has not affected the CHISM.…”

Section: Heliospheric Ismsupporting

confidence: 71%

Is the Sun Embedded in a Typical Interstellar Cloud?

Frisch

2008

From the Outer Heliosphere to the Local Bubble

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The physical properties and kinematics of the partially ionized interstellar material (ISM) near the Sun are typical of warm diffuse clouds in the solar vicinity. The direction of the interstellar magnetic field at the heliosphere, the polarization of light from nearby stars, and the kinematics of nearby clouds are naturally explained in terms of the S1 superbubble shell. The interstellar radiation field at the Sun appears to be harder than the field ionizing ambient diffuse gas, which may be a consequence of the low opacity of the tiny cloud surrounding the heliosphere. The spatial context of the Local Bubble is consistent with our location in the Orion spur.

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“…3 (Gloeckler and Wenzel 2001;. Helium isotopes show 4 He/ 3 He ∼ 1.7 × 10 −4 , which is similar to meteoritic and HII region values (Salerno et al 2003;Gloeckler and Fisk 2007). These data suggest the CHISM composition is solar, independent of uncertainties in actual solar abundances.…”

Section: Pickup Ions and Anomalous Cosmic Rayssupporting

confidence: 77%

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

et al. 2009

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Interstellar material (ISMa) is observed both inside and outside of the heliosphere. Relating these diverse sets of ISMa data provides a richer understanding of both the interstellar medium and the heliosphere. The galactic environment of the Sun is dominated by warm, low-density, partially ionized interstellar material consisting of atoms and dust grains. The properties of the heliosphere are dependent on the pressure, composition, radiation field, ionization, and magnetic field of ambient ISMa. The very low-density interior of the Local Bubble, combined with an expanding superbubble shell associated with star formation in the Scorpius-Centaurus Association, dominate the properties of the local interstellar medium (LISM). Once the heliosphere boundaries and interaction mechanisms are understood, interstellar gas, dust, pickup ions, and anomalous cosmic rays inside of the heliosphere can be directly compared to ISMa outside of the heliosphere. Our understanding of ISMa at the Sun is further enriched when the circumheliospheric interstellar material is compared to observations of other nearby ISMa and the overall context of our galactic environment. The IBEX mission will map the interaction region between the heliosphere and ISMa, and improve the accuracy of comparisons between ISMa inside and outside the heliosphere.

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Measurement of³He/⁴He in the Local Interstellar Medium: the Collisa Experiment onMir

Cited by 20 publications

References 22 publications

Is the Sun Embedded in a Typical Interstellar Cloud?

Is the Sun Embedded in a Typical Interstellar Cloud?

Is the Sun Embedded in a Typical Interstellar Cloud?

The Galactic Environment of the Sun: Interstellar Material Inside and Outside of the Heliosphere

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