نجمي متوسط

The distribution of ionized hydrogen (known by astronomers as H II from old spectroscopic terminology) in the parts of the Galactic interstellar medium visible from the Earth's northern hemisphere as observed with the Wisconsin Hα Mapper (Haffner et al. 2003).

النجمي المتوسط Interstellar medium أوالحبيبة بين نجمية هى جسيم غبارى سديمي يسبب الخمود بين النجمي وهى صغيرة جدا يبغ قطرها 1\10,000 ملمتر ويعتقد حتى هذة الحبيبات تحتوى على الكربون على الأكثر.

المسألة بين النجوم

**Table 1: Components of the interstellar medium**
Component	Fractional Volume	Scale Height (pc)	Temperature (K)	Density (atoms/cm³)	State of hydrogen	Primary observational techniques
Molecular clouds	< 1%	70	10—20	10²—10⁶	molecular	Radio and infrared molecular emission and absorption lines
Cold Neutral Medium (CNM)	1—5%	100—300	50—100	20—50	neutral atomic	H I 21 cm line absorption
Warm Neutral Medium (WNM)	10—20%	300—400	6000—10000	0.2—0.5	neutral atomic	H I 21 cm line emission
Warm Ionized Medium (WIM)	20—50%	1000	8000	0.2—0.5	ionized	Hα emission and pulsar dispersion
H II regions	< 1%	70	8000	10²—10⁴	ionized	Hα emission and pulsar dispersion
Coronal gas Hot Ionized Medium (HIM)	30—70%	1000—3000	10⁶—10⁷	10⁻⁴—10⁻²	ionized (metals also highly ionized)	X-ray emission; absorption lines of highly ionized metals, primarily in the ultraviolet

التفاعل مع الوسط بين الكواكب

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Schematic diagram of the interaction between the ISM and the interplanetary medium

التدفئة والتبريد

التاريخ

انظر أيضا

سديم
خمود بين نجمي

List of molecules in interstellar space
Diffuse interstellar band
Photodissociation region
Interstellar masers
Interplanetary medium
Heliosphere
Outer Solar System
Outer space
Stellar system
Timeline of knowledge about the interstellar and intergalactic medium

ملاحظات

^ Based on Table 1 of Ferriere (2001), with additional details from the text of the same paper.

المصادر

مؤمن, عبد الأمير (2006). قاموس دار الفهم الفلكي. بيروت، لبنان: دار الفهم للملايين.

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