NGC 40 (also known as the Bow-Tie Nebula and Caldwell 2) is a planetary nebula composed of hot gas around a dying star. The star has ejected its outer layer which has left behind a small, hot star. Radiation from the star causes the shed outer layer to heat to about 10,000 degrees Celsius and become visible as a planetary nebula. The nebula is about one light-year across at a distance of 2 700 light-years. About 30 000 years from now, scientists theorize that NGC 40 will fade away, leaving only a white dwarf star approximately the size of Earth.
Morphologically, the shape of NGC 40 resembles a barrel with the long axis pointing towards the north-northeast. There are two additional pairs of lobes around the poles, which correspond to additional ejections from the star.
The central star of NGC 40 (HD 826) has a spectral type of [WC8], indicating a spectrum similar to that of a carbon-rich Wolf–Rayet star. The central star has a bolometric luminosity of about 7 000 L☉ and radius of 0.56 R☉. The star appears to have an effective temperature of about 71 000 K, but the temperature of the source ionizing the nebula is only about 45 000 K. One proposed explanation to this contradiction is that the star was previously cooler, but has experienced a late thermal pulse which re-ignited fusion and caused its temperature to increase.
NGC 40, Bow Tie Nebula
NGC 40 (also known as the Bow-Tie Nebula and Caldwell 2) is a planetary nebula composed of hot gas around a dying star. The star has ejected its outer layer which has left behind a small, hot star. Radiation from the star causes the shed outer layer to heat to about 10,000 degrees Celsius and become visible as a planetary nebula. The nebula is about one light-year across at a distance of 2 700 light-years. About 30 000 years from now, scientists theorize that NGC 40 will fade away, leaving only a white dwarf star approximately the size of Earth.
Morphologically, the shape of NGC 40 resembles a barrel with the long axis pointing towards the north-northeast. There are two additional pairs of lobes around the poles, which correspond to additional ejections from the star.
The central star of NGC 40 (HD 826) has a spectral type of [WC8], indicating a spectrum similar to that of a carbon-rich Wolf–Rayet star. The central star has a bolometric luminosity of about 7 000 L☉ and radius of 0.56 R☉. The star appears to have an effective temperature of about 71 000 K, but the temperature of the source ionizing the nebula is only about 45 000 K. One proposed explanation to this contradiction is that the star was previously cooler, but has experienced a late thermal pulse which re-ignited fusion and caused its temperature to increase.
Photographed with the RC8″ reflector telescope and the ASI 2600MC CMOS color camera in Stuvsta, September 15th, 2024. Exposure was 39 * 2 min with IDAS LPS P3 light pollution filter. Postprocesssing in Pixinsight with Blur XTerminator.
NGC 40, Bow Tie Nebula
NGC 40 (also known as the Bow-Tie Nebula and Caldwell 2) is a planetary nebula composed of hot gas around a dying star. The star has ejected its outer layer which has left behind a small, hot star. Radiation from the star causes the shed outer layer to heat to about 10,000 degrees Celsius and become visible as a planetary nebula. The nebula is about one light-year across at a distance of 2 700 light-years. About 30 000 years from now, scientists theorize that NGC 40 will fade away, leaving only a white dwarf star approximately the size of Earth.
Morphologically, the shape of NGC 40 resembles a barrel with the long axis pointing towards the north-northeast. There are two additional pairs of lobes around the poles, which correspond to additional ejections from the star.
The central star of NGC 40 (HD 826) has a spectral type of [WC8], indicating a spectrum similar to that of a carbon-rich Wolf–Rayet star. The central star has a bolometric luminosity of about 7 000 L☉ and radius of 0.56 R☉. The star appears to have an effective temperature of about 71 000 K, but the temperature of the source ionizing the nebula is only about 45 000 K. One proposed explanation to this contradiction is that the star was previously cooler, but has experienced a late thermal pulse which re-ignited fusion and caused its temperature to increase.
Photographed with the RC8″ reflector telescope and the ASI 2600MC CMOS color camera in Stuvsta, September 15th, 2024. Exposure was 39 * 2 min with IDAS LPS P3 light pollution filter. Postprocesssing in Pixinsight with Blur XTerminator.
NGC 40, Bow Tie Nebula
NGC 40 (also known as the Bow-Tie Nebula and Caldwell 2) is a planetary nebula composed of hot gas around a dying star. The star has ejected its outer layer which has left behind a small, hot star. Radiation from the star causes the shed outer layer to heat to about 10,000 degrees Celsius and become visible as a planetary nebula. The nebula is about one light-year across at a distance of 2 700 light-years. About 30 000 years from now, scientists theorize that NGC 40 will fade away, leaving only a white dwarf star approximately the size of Earth.
Morphologically, the shape of NGC 40 resembles a barrel with the long axis pointing towards the north-northeast. There are two additional pairs of lobes around the poles, which correspond to additional ejections from the star.
The central star of NGC 40 (HD 826) has a spectral type of [WC8], indicating a spectrum similar to that of a carbon-rich Wolf–Rayet star. The central star has a bolometric luminosity of about 7 000 L☉ and radius of 0.56 R☉. The star appears to have an effective temperature of about 71 000 K, but the temperature of the source ionizing the nebula is only about 45 000 K. One proposed explanation to this contradiction is that the star was previously cooler, but has experienced a late thermal pulse which re-ignited fusion and caused its temperature to increase.
Photographed with the RC8″ reflector telescope and the ASI 2600MC CMOS color camera in Stuvsta, September 15th, 2024. Exposure was 39 * 2 min with IDAS LPS P3 light pollution filter. Postprocesssing in Pixinsight with Blur XTerminator.
