Salvato in:
| Autori principali: | , , , , , , , , , , , , , , , , , , , , , , , , , , , |
|---|---|
| Natura: | Preprint |
| Pubblicazione: |
2025
|
| Soggetti: | |
| Accesso online: | https://arxiv.org/abs/2508.15900 |
| Tags: |
Aggiungi Tag
Nessun Tag, puoi essere il primo ad aggiungerne!!
|
| _version_ | 1866910018025029632 |
|---|---|
| author | Craig, Peter Aydi, Elias Chomiuk, Laura Stone, Ashley Strader, Jay Chong, Atticus Li, Kwan-Lok Fan, Jhih-Ling Bahramian, Arash Buckley, David A. H. Izzo, Luca Kawash, Adam Metzger, Brian D. Mukai, Koji Linford, Justin D. Orio, Marina Sokoloski, J. L. Sokolovsky, Kirill V. Tremou, Evangelia Walter, Frederick M. Fló, Joan Guarro Boussin, Christophe Charbonne, Stéphane Garde, Olivier Belyakov, Konstantin Monard, Libert A. G. Hambsch, Franz-Josef Thomas, Neil |
| author_facet | Craig, Peter Aydi, Elias Chomiuk, Laura Stone, Ashley Strader, Jay Chong, Atticus Li, Kwan-Lok Fan, Jhih-Ling Bahramian, Arash Buckley, David A. H. Izzo, Luca Kawash, Adam Metzger, Brian D. Mukai, Koji Linford, Justin D. Orio, Marina Sokoloski, J. L. Sokolovsky, Kirill V. Tremou, Evangelia Walter, Frederick M. Fló, Joan Guarro Boussin, Christophe Charbonne, Stéphane Garde, Olivier Belyakov, Konstantin Monard, Libert A. G. Hambsch, Franz-Josef Thomas, Neil |
| contents | Classical novae in the Milky Way have now been well-established as high-energy GeV $γ$-ray sources. In novae with main-sequence companions, this emission is believed to result from shocks internal to the nova ejecta, as a later fast wind collides with an earlier slow outflow. To test this model and constrain the $γ$-ray production mechanism, we present a systematic study of a sample of recent Galactic novae, comparing their $γ$-ray properties ($γ$-ray luminosity and duration) with their outflow velocities, peak $V$-band magnitudes, and the decline times of their optical light curves ($t_2$). We uniformly estimate distances in a luminosity-independent manner, using spectroscopic reddening estimates combined with three-dimensional Galactic dust maps. Across our sample, $γ$-ray luminosities ($>$100 MeV) vary by three orders of magnitude, spanning $10^{34}-10^{37}$ erg s$^{-1}$. Novae with larger velocity of the fast outflow (or larger differential between the fast and slow outflow) have larger $γ$-ray luminosities, but are detectable for a shorter duration. The optical and $γ$-ray fluxes are correlated, consistent with substantial thermal emission in the optical from shock-heated gas. Across six novae with $γ$-ray and infrared light curves, evidence for dust formation appears soon after the end of the detected $γ$-ray emission. Dusty and non-dusty novae appear to have similar $γ$-ray luminosities, though novae that have more material processed by the shocks may be more likely to form dust. We find that the properties of the $γ$-ray emission in novae depend heavily on the ejecta properties, and are consistent with expectations for internal shocks. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_15900 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | What determines the $γ$-ray luminosities of classical novae? Craig, Peter Aydi, Elias Chomiuk, Laura Stone, Ashley Strader, Jay Chong, Atticus Li, Kwan-Lok Fan, Jhih-Ling Bahramian, Arash Buckley, David A. H. Izzo, Luca Kawash, Adam Metzger, Brian D. Mukai, Koji Linford, Justin D. Orio, Marina Sokoloski, J. L. Sokolovsky, Kirill V. Tremou, Evangelia Walter, Frederick M. Fló, Joan Guarro Boussin, Christophe Charbonne, Stéphane Garde, Olivier Belyakov, Konstantin Monard, Libert A. G. Hambsch, Franz-Josef Thomas, Neil High Energy Astrophysical Phenomena Classical novae in the Milky Way have now been well-established as high-energy GeV $γ$-ray sources. In novae with main-sequence companions, this emission is believed to result from shocks internal to the nova ejecta, as a later fast wind collides with an earlier slow outflow. To test this model and constrain the $γ$-ray production mechanism, we present a systematic study of a sample of recent Galactic novae, comparing their $γ$-ray properties ($γ$-ray luminosity and duration) with their outflow velocities, peak $V$-band magnitudes, and the decline times of their optical light curves ($t_2$). We uniformly estimate distances in a luminosity-independent manner, using spectroscopic reddening estimates combined with three-dimensional Galactic dust maps. Across our sample, $γ$-ray luminosities ($>$100 MeV) vary by three orders of magnitude, spanning $10^{34}-10^{37}$ erg s$^{-1}$. Novae with larger velocity of the fast outflow (or larger differential between the fast and slow outflow) have larger $γ$-ray luminosities, but are detectable for a shorter duration. The optical and $γ$-ray fluxes are correlated, consistent with substantial thermal emission in the optical from shock-heated gas. Across six novae with $γ$-ray and infrared light curves, evidence for dust formation appears soon after the end of the detected $γ$-ray emission. Dusty and non-dusty novae appear to have similar $γ$-ray luminosities, though novae that have more material processed by the shocks may be more likely to form dust. We find that the properties of the $γ$-ray emission in novae depend heavily on the ejecta properties, and are consistent with expectations for internal shocks. |
| title | What determines the $γ$-ray luminosities of classical novae? |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.15900 |