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Sternbild SCHIFFSHECK ( Puppis -Puppis – Pup ) Nördlicher Teil (Bis -34° Dekl.)

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Sternbild SCHIFFSHECK ( Puppis -Puppis – Pup ) Nördlicher Teil (Bis -34° Dekl.) Sternbild SCHIFFSHECK ( Puppis -Puppis – Pup ) nördlicher Teil (bis -34° Dekl.) Das SCHIFFSHECK wird auch als Achterschiff oder Hinterdeck bezeichnet. Es ist ein Sternbild des südlichen Himmels und der größte Teil des ursprünglichen Sternbildes SCHIFF ARGO (Argo Narvis), ein ausgedehntes Sternbild am Südhimmel, das das griechische Schiff der Argonautensage um Jason darstellen soll. Es bestand aus den 4 heutigen Sternbildern SCHIFFSHECK (PUPPIS), SCHIFFSKIEL (CARINA), SEGEL (VELA) und KOMPASS (PYXIS). Das „Heck“ befindet sich im Bereich des Milchstraßenbandes und enthält sternreiche Objekte- vor allem fernglastaugliche Offene Sternhaufen. In unseren Breiten ist leider nur der nördliche Teil des Sternbildes einsehbar. Das Schiffsheck kulminiert im Januar gegen 24:00Uhr. Es befindet sich innerhalb der Koordinaten RE 06h02’ bis 08h28’ und DE –11°15' bis –51°06' und nimmt am Himmel eine Fläche von 673°2 ein. Es grenzt im Norden an WASSERSCHLANGE und EINHORN, im Westen an GROSSER HUND, TAUBE und MALER, im Süden an MALER und SCHIFFSKIEL, im Osten an SEGEL, KOMPASS und WASSERSCHLANGE. Das Schiffsheck ist südlich von –78° geografischer Breite zirkumpolar und nördlich von 39° nicht mehr vollständig sichtbar. Die Objekte: 1. Das „Hinterdeck“ 2. Doppelsterne 3. Veränderliche 4. Die hellsten Offenen Sternhaufen 1. Die Sterne vom Hinterdeck: 8 Sterne 2. und 3. Größenklasse, Rho – Xi „Azmidiske“ – k1+2 – Pi – Ny – Tau – Sigma und Zeta „Naos“ markieren das „Hinterteil“ des gesamten „Schiff Argo“- Komplexes. Es sind in diesem Sternbild die hellsten Sterne. Leider können wir von unserem mitteleuropäischen Standpunkt aus nur bis zu den Sterne Rho, Xi und k1+2 beobachten. Der größte Teil des „Hecks“ steht unter dem Horizont. TUREIS, Rho (ρ) Puppis, 15 Pup; RE 08h 07' 33“ / DE -24° 18' arab. „Schild“; mv= 2,83mag; Spektrum= F6IIp; Distanz= 62,73LJ; LS= 23fach; Mv= 1,4Mag; MS= 1,9fach; RS= 3,7fach; OT= 6540K; RoD= 13 Tage; RoG= 14km/s; EB= 0,100“/Jhr; RG= +46,1km/s; Alter ca. 2Mrd. Jahre; Mehrfachsystem; Komponente A= spektrobinär; Orbitperiode= 0,141 Tage; Spektrum Komponente B= M5V; mittlere Halbachse= 30“ (570AE= 85,5Mrd. km); Orbitdauer ca. 1000 Jahre δSct- veränderlich (Zwergcepheid); Amplitude= 2,68mag – 2,78mag. AZMIDISKE, Xi (ξ) Puppis, 7 Pup; RE 07h 49' 18“ / DE -24° 51' auch Aspidiske, lat. „Kleines Schild“; mv= 3,34mag; Spektrum= G6Ia; Distanz= 1350LJ; LS= 6600fach; Mv= - 4,7Mag; MS= 9,9fach;RS= 120fach; OT= 4990K; EB= 0,008“/Jhr.; RG= +2,7km/; Alter ca. 26,7Mill. Jahre; Mehrfachsystem; siehe Doppelsterne MARKEB, k1 +k2 Puppis; RE 07h 38' 50“ / DE -26° 48' k1 Puppis: mv= 4,51mag; Spektrum= B6IV; Distanz= 454LJ; LS= 480fach; Mv= -1,8Mag; MS= ; RS= ; OT= ; RoD= ; RoG= km/s; EB= 0,026“/Jhr.; RG= +33,0km/s; Alter ca. ; Kappa hat einen ebenbürtigen Partner in 10“ Distanz; siehe 3. Doppelsterne k2 Puppis: mv= 4,62mag; Spektrum= B5IV; Distanz= 462LJ; LS= 490fach; Mv= -1,9Mag; Die Gesamthelligkeit von k Puppis beträgt 3,80mag; Siehe 3. Doppelsterne 3. Doppelsterne Xi Puppis „Azmidiske“, RE 07h 49' 18“ / DE -24° 51'; Gesamthelligkeit 3,34mag Komponente A= spektrobinär; mittlere Halbachse Aa - Ab= 2AE (300Mill. km); Orbitperiode= ca. 1 Jahr. mv Komponenten A + B= 3,34mag + 13,00mag; Spektren= G6Ia + M2V; Distanz A-B= 5“; mittlere Halbachse A - B= 2000AE (300Mrd. km); Orbitdauer ca. 26000 Jahre; optisch doppelt mit HD 63669; mv Komponenten A + B (HD 63669)= 3,30mag + 5,30mag; Spektren= G5Ia + G0III; Distanz Komponente B (HD 63669)= 321LJ; LS= 60fach; Mv= 0,4Mag; EB= 0,036“/Jhr.; RG= +1,6km/s; Distanz A-B= 288“; PW= 229° (1991); Siehe 1. „Das Hinterdeck“ k1+2 Puppis „Markeb“, RE 07h 38' 50“ / DE -26° 48'; Gesamthelligkeit 3,80mag mv Komponenten A + B= 4,40mag + 4,62mag; Spektren= B5IV + B6V; Distanz A-B= 10,2“; PW= 317° (2009); Komponente B ist ebenfalls doppelt; mv Komponenten B + C= 4,62mag + 13,80mag; Distanz B-C= 7,2“; PW= 222° (1927); Siehe 1. „Das Hinterdeck“ HD 64379; RE 07h 52' 16“ / DE -34° 42“; Gesamthelligkeit 5,01mag Spektrum= F3/F5V; Distanz= 58,79LJ; LS= 2,7fach; Mv= 3,7Mag; EB= 0,313“/Jhr.; RG= +26,7km/s; zur Hyadengruppe mv Komponenten A + B= 5,12mag + 8,59mag; Spektren= F3V + F5V; Distanz A-B= 3,8“; PW= 267° (2001); OS Puppis, RE 08h 13' 58“ / DE -36° 19' mv= 5,09mag; Spektrum= B2V; Distanz= 1180LJ; LS= 1009fach; Mv= -2,7Mag; EB= 0,006“/Jhr.; RG= +18,0km/s; mv Komponenten A + B= 4,10mag + 6,01mag; Spektren= B3V + B8V; Distanz A-B= 67,4“; PW= 175° (2009); γC- veränderlich; Amplitude= 5,07mag – 5,20mag; Periode= irregulär; 5 Puppis, RE 07h 47' 57“ / DE -12° 11'; Gesamthelligkeit 5,48mag mv= 5,48mag; Spektrum= F5+...; Distanz= 98,7LJ; LS= 5fach; Mv= 3,1Mag; MS= 1,5fach; RS= 1,6fach; OT= 6607K; EB= 0,129“/Jhr.; RG= +27,4km/s; mv Komponenten A + B= 5,73mag + 7,32mag; Spektren= F5V + G3V; Distanz A-B= 1,1“; PW= 340° (2014); 4. Die Veränderlichen Sterne Rho Puppis „Tureis“, RE RE 08h 07' 33“ / DE -24° 18', mittlere Helligkeit 2,83mag; Typ δSct (Zwergcepheide); Amplitude= 2,68mag – 2,87mag; Periode= o,141 Tage, ´ Siehe 1. „Das Hinterdeck“ MX Puppis, RE 08h 13' 30“ / DE -35° 54', mittlere Helligkeit 4,78mag mv= 4,78mag; Spektrum= B1,5IIIe; Distanz= 980LJ; LS= 920fach; Mv= -2,6Mag; MS= 10,1fach; RS= 9fach; OT= 25172K; EB= 0,005“/Jhr.; RG= +35,0km/s; Alter ca. 22,5Mill. Jahre; zur Pup OB3 Assoziation; Typ γC, Hüllenstern; Amplitude= 4,60mag – 4,92mag; Periode= irr.; 5. Die hellsten Offenen Sternhaufen M46, NGC 2437; RE 07° 41‘ 47“ / DE –14° 48‘; Typ II2r; mv= 6,1mag; D= 27‘; wahrer D= 30LJ; Distanz ca. 5.400 LJ; RG= +48,1km/s; etwa 150 Sterne ab 8,7mag; Alter etwa 300 Mill. Jahre; Im Nebel befindet sich der PN NGC 2438: Typ 4,2; D= 1,1‘; ZS= 17,7mag) M46 ist ein sehr reicher Haufen mit über 150 Sternen ab 10 - 13mag und mit einer Gesamtzahl von möglicherweise über 500. Die hellsten Sterne gehören zu der Spektralklasse A0, jeder von diesen ist 100 Mal leuchtkräftiger als die Sonne. Das deutet auf ein Alter von etwa 300 Millionen Jahren. Die Sterne sind über ein Gebiet von einem Winkeldurchmesser von 27 Bogenminuten verstreut, was einer Ausdehnung von etwa 30 Lichtjahren entspricht; der Sternhaufen entfernt sich von uns mit einer Geschwindigkeit von 48,1 km/s. M46 befindet sich etwa 5° südlich vom Stern Alpha Mon (3,9mag). Etwa 1° westlich sehen wir den OH M47. M46 ist ein heller Nebel im Fernglas und im Teleskop äußerst beeindruckend Der hellste Stern hat 8,7 Magnituden. Der Haufen zeigt eine ovale Struktur. Im nördlichen Teil von M46 befindet sich der Planetarische Nebel NGC 2438. Er gehört wahrscheinlich nicht zum Haufen. Seine Distanz beträgt etwa 4.000 LJ. Die Koordinaten des PN: 07h 41‘ 51“ / DE –14° 44. M47, NGC 2422; RE 07h 36‘ 35“ / -14° 29‘; Typ III2m; mv= 4,4mag; D= 30‘; wahrer D= 12LJ; Distanz ca. 1.600 LJ; RG= +37km/s; Alter etwa 78 Mill. Jahre; etwa 50 Sterne ab 5,7mag; M47 ist, wie sein „linker Kollege“ M46, ein beeindruckender Fernglashaufen., kaum besser im Teleskop. Er ist schon mit freiem Auge als kleines Nebelfleckchen sichtbar und zeigt zumeist helle Sterne.. Es handelt sich um einen grobkörnigen Haufen mit 50 Sterne in einer Region von 12 Lichtjahren Durchmesser verstreut. Der hellste Stern gehört zur Spektralklasse B2 und ist 5.7mag hell; die gesamte Sternpopulation ähnelt den Plejaden. M 47 enthält auch zwei orangefarbene K- Riesen mit jeweils einer Leuchtkraft, die die der Sonne um das 200-fache übersteigt. Der Sky Catalog 2000 gibt ein geschätztes Alter von 78 Millionen Jahren für diesen Sternenschwarm an, der sich von uns mit einer Geschwindigkeit von37 km/s entfernt. Der helle Stern nahe dem Zentrum auf unserem Bild ist der schöne Doppelstern Sigma 1121, dessen Komponenten beide 7.9mag haben und 7.4 Bogensekunden voneinander getrennt sind. M93, NGC 2447; RE 07h 44‘ 29“ / DE –23° 51‘; Typ I3r; mv= 6,2mag; D= 22‘; wahrer D= 23LJ; Distanz ca. 3.600 LJ; RG= 21,3km/s; etwa 80 Sterne ab 8,2mag; Alter etwa 98 Mill. Jahre; M93 befindet sich etwa 1,5° in Richtung 1h von Xi Pup AZMIDISKE (3,2mag). Es ist im Teleskop ein wunderschön aufgelöster Sternhaufen, der drei parallele Sternketten aufweist. Man kann etwa 80 Sterne ab 8,2mag beobachten. M 93 gehört zu den kleineren, aber hellen offenen Sternhaufen; seine Sterne bilden ein Dreieck förmiges Gebilde. Zum Haufen gehören mindestens 80 Mitglieder, die sich über ein Gebiet von 22 Bogenminuten Durchmesser verteilen, das entspricht etwa einer linearen Ausdehnung von 20 bis 25 LJ. Die hellsten Sterne von M93 sind blaue Riesen des Spektraltyps B9. Das Alter des Haufens wird auf knapp 100 Millionen Jahre geschätzt. .
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