Top Tweets for #m97
Meine kleine Eule ist zu kurz gekommen, jetzt wollte sie endlich mal in die Nacht fliegen! 🙂#M97 mit Seestar S50 #OwlNebula🦉
17時台有難うございました！
18:30から #FMさつませんだい
#げそ太郎の一期一笑
今日は、 セレクトショップ #enさん
そして、そしてフードトラック #M97
さんをご紹介します！✨✨
素敵なイベントの情報もお届けしますよ！
是非お聴きください！
インスタライブも是非✨✨
If #Leapmotor L orders #NIO #M97 chip
➡️could open door to #Stellantis S, 20% stake of L
S=parent comp of 14 brands (additional to >20 Geely brands): #Abarth #AlfaRomeo #Chrysler #Citroën #DSAutomobiles #Dodge #Fiat #Jeep #Lancia #Maserati #Opel #Peugeot
https://t.co/mKVgOXqwz5
昨夜撮影したM97です。
いやー、さすがにこれは小さ過ぎるなー😅
今の状態だと拡大してもザラザラだしちょっと無理がありそうですね🥹
右上にはM108もちゃっかり写り込んでおります！
#M97
今日も一日、お疲れ様でした！
約1800光年の彼方にある、惑星状星雲M97（ふくろう星雲）です。（'25年5月4日21時30分、BORG76ED、Canon EOS 7D MarkⅡで撮影）
#写真好きな人と繋がりたい
#星好きな人と繋がりたい
#東京カメラ部 #tokyocameraclub #M97 #ふくろう星雲
Als ich nach Hause kam, schaute Orion zum Balkon herein, kramte schnell Seestar S50 heraus und los ging's! Es kamen Wolken und ich wechselte zu #M97, gerade noch etwas geschnappt, dann kamen auch im Osten die Wolken! Zu wenig Daten, obwohl ich noch eine alte🦉dazu tat!🦉1🌟center
#M97 — The Owl Nebula (NGC 3587)
**Type:** Planetary Nebula
**Constellation:** Ursa Major
**Right Ascension:** 11h 14m 47.7s
**Declination:** +55° 01′ 08″
**Distance:** ~2.0–2.6 thousand light-years
**Angular Diameter:** ~3.4 arcminutes
**Integrated Magnitude:** ~9.9
**Central Star Magnitude:** ~16
---
## **1. Origin and Evolution**
The Owl Nebula is the ionized envelope of a ~2–3 M⊙ star that shed its outer layers during the asymptotic giant branch (AGB) phase. Ultraviolet radiation from the remaining white dwarf ionizes the material, producing the nebula’s characteristic glow.
- **Dynamical age:** ~6000 years
- **Central star:** ~0.6–0.7 M⊙ white dwarf
- **Expansion velocity:** 25–40 km/s
- **Ionized mass:** ~0.1–0.3 M⊙
---
## **2. Morphology and Structure**
### **Inner Cavities (“Eyes”)**
Two low-density holes carved by fast stellar winds give the nebula its “owl face” appearance.
### **Main Shell**
Predominantly spherical but actually slightly triaxial. Strongly emits in [O III], outlining the brighter membrane.
### **Outer Halo**
A very faint halo extending to ~8–10 arcminutes traces earlier mass-loss episodes from the progenitor star.
---
## **3. Physical Scale**
At ~2.03 kly, the ~3.4′ diameter corresponds to:
**≈ 2 light-years across**
---
## **4. Spectroscopic Characteristics**
The nebula’s spectrum arises from photoionized gas surrounding the central white dwarf.
### **Strongest Emission Lines**
- **[O III] 4959 & 5007 Å**
- **Hα 6563 Å**
- **[N II] 6548 & 6583 Å**
- **He II 4686 Å**
### **Plasma Conditions**
- **Electron temperature:** 10,000–13,000 K
- **Electron density:** 100–1000 cm⁻³
Abundance patterns show enhanced helium and nitrogen from stellar nucleosynthesis during the AGB phase.
---
## **5. Kinematics and Dynamics**
- The nebula expands at **25–40 km/s**, depending on ionic species.
- Velocity splitting in [O III] and Hα reveals internal asymmetries.
- Shaping results from the interaction between:
1. A slow AGB wind
2. A later, fast post-AGB wind
These processes sculpt the cavities and overall shell geometry.
---
## **6. Scientific Significance**
- A benchmark planetary nebula for studying **anisotropic mass loss**.
- Shows pronounced **ionization stratification** useful in modeling photoionization fronts.
- The halo preserves the mass-loss history over ~10⁴ years.
- One of the most extensively studied nebulae in the northern sky.
---
## **7. Selected References (Peer-Reviewed)**
1. Guerrero, M.A. et al. 2003, *A&A*, 412, 41
2. O’Dell, C.R. et al. 2002, *AJ*, 123, 3329
3. Ragazzoni, R. et al. 2001, *A&A*, 369, 1083
4. Reay, N.K. & Atherton, P.D. 1983, *MNRAS*, 202, 17P
5. Sabbadin, F. et al. 1984, *A&A*, 136, 341
6. Stanghellini, L. et al. 2010, *ApJ*, 714, 1096
7. Steffen, W. et al. 2014, *MNRAS*, 442, 3316
![BobMcGwier_N4HY's tweet photo. #M97 — The Owl Nebula (NGC 3587)
**Type:** Planetary Nebula
**Constellation:** Ursa Major
**Right Ascension:** 11h 14m 47.7s
**Declination:** +55° 01′ 08″
**Distance:** ~2.0–2.6 thousand light-years
**Angular Diameter:** ~3.4 arcminutes
**Integrated Magnitude:** ~9.9
**Central Star Magnitude:** ~16
---
## **1. Origin and Evolution**
The Owl Nebula is the ionized envelope of a ~2–3 M⊙ star that shed its outer layers during the asymptotic giant branch (AGB) phase. Ultraviolet radiation from the remaining white dwarf ionizes the material, producing the nebula’s characteristic glow.
- **Dynamical age:** ~6000 years
- **Central star:** ~0.6–0.7 M⊙ white dwarf
- **Expansion velocity:** 25–40 km/s
- **Ionized mass:** ~0.1–0.3 M⊙
---
## **2. Morphology and Structure**
### **Inner Cavities (“Eyes”)**
Two low-density holes carved by fast stellar winds give the nebula its “owl face” appearance.
### **Main Shell**
Predominantly spherical but actually slightly triaxial. Strongly emits in [O III], outlining the brighter membrane.
### **Outer Halo**
A very faint halo extending to ~8–10 arcminutes traces earlier mass-loss episodes from the progenitor star.
---
## **3. Physical Scale**
At ~2.03 kly, the ~3.4′ diameter corresponds to:
**≈ 2 light-years across**
---
## **4. Spectroscopic Characteristics**
The nebula’s spectrum arises from photoionized gas surrounding the central white dwarf.
### **Strongest Emission Lines**
- **[O III] 4959 & 5007 Å**
- **Hα 6563 Å**
- **[N II] 6548 & 6583 Å**
- **He II 4686 Å**
### **Plasma Conditions**
- **Electron temperature:** 10,000–13,000 K
- **Electron density:** 100–1000 cm⁻³
Abundance patterns show enhanced helium and nitrogen from stellar nucleosynthesis during the AGB phase.
---
## **5. Kinematics and Dynamics**
- The nebula expands at **25–40 km/s**, depending on ionic species.
- Velocity splitting in [O III] and Hα reveals internal asymmetries.
- Shaping results from the interaction between:
1. A slow AGB wind
2. A later, fast post-AGB wind
These processes sculpt the cavities and overall shell geometry.
---
## **6. Scientific Significance**
- A benchmark planetary nebula for studying **anisotropic mass loss**.
- Shows pronounced **ionization stratification** useful in modeling photoionization fronts.
- The halo preserves the mass-loss history over ~10⁴ years.
- One of the most extensively studied nebulae in the northern sky.
---
## **7. Selected References (Peer-Reviewed)**
1. Guerrero, M.A. et al. 2003, *A&A*, 412, 41
2. O’Dell, C.R. et al. 2002, *AJ*, 123, 3329
3. Ragazzoni, R. et al. 2001, *A&A*, 369, 1083
4. Reay, N.K. & Atherton, P.D. 1983, *MNRAS*, 202, 17P
5. Sabbadin, F. et al. 1984, *A&A*, 136, 341
6. Stanghellini, L. et al. 2010, *ApJ*, 714, 1096
7. Steffen, W. et al. 2014, *MNRAS*, 442, 3316](https://pbs.twimg.com/media/G6DXvSqWoAADLby.jpg)
今日という日が素晴らしい一日でありますように！
1800光年の彼方にあるフクロウ星雲M97（スマート望遠鏡DWARF３で撮影）と通勤途上の花々です。
#写真好きな人と繋がりたい
#花好きな人と繋がりたい
#星好きな人と繋がりたい
#野の花 #道端の花 #M97 #スマート望遠鏡 #DWARF3 #DWARFLABjp
#OwlNebula #M97 #Astrophotography #Askar103APO
小さいM97をDrizzle3xで解像度を上げ，DynamicCropで３倍にクロップするとそれなりの大きさ。解像度を上げているのでさらに拡大して見ても，ざらつきは少ない。
M97 (Owl Nebula) is a luminous planetary nebula located about 2,030 light years away in Ursa Major. The structure formed around 8,000 years ago from the outflow of material emitted by stellar winds from its central star as it evolved along the asymptotic giant branch.📷NASA #M97
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