Hyperboreae Undae (Latin: "Far Northern Waves/Dunes") is one of the largest and densest dune fields of Planum Boreum, the Martian North Pole. It is named after one of the classical albedo features on Mars. Its name was officially approved by IAU in 1988. It extends from latitude 77.12°N to 82.8°N and from longitude 302.92°E to 316.02°E (43.98°W – 57.08°W). Its centre is at latitude 79.96°N, longitude 49.49°W, and has a diameter of 463.65 kilometres (288.10 mi).

Hyperboreae Undae is southwest of the Boreum Cavus depression, an arc-like depression at the northeastern boundary of Chasma Boreale. From there, Hyperboreae Undae continues in a southwestern direction through Chasma Boreale, and into the lowlands of Vastitas Borealis. It overlays the eastern part of Hyperboreae Lingua and the region above Escorial crater.

Hyperboreae Undae is well known for the barchanoid and linear dunes that have formed at its location, although they are seemingly incompatible. Research has been ongoing to explain the coexistence of these types of dunes at Hyperboreae Undae and elsewhere on Mars. Another type of formation found at Hyperboreae Undae is the yardang.

Although the dunes surrounding the Martian north pole show no signs of movement, two possible exceptions may be the dunes in parts of Abalos Undae, and the dunes of Hyperboreae Undae. In the case of Hyperboreae Undae, the dunes close to its eastern boundary appear to be buried under the Planum Boreum 3 unit. At that area, some of the dunes exhibit dark streaks that may have been caused by katabatic winds. This may indicate sand movement, due to Aeolian activity, which is recent enough to retain the streaks, otherwise these marks tend to disappear with time; other dunes do not exhibit such marks.

The dunes of Hyperboreae Undae, according to data provided by the Compact Reconnaissance Imaging Spectrometer for Mars, exhibit the weakest signature for the presence of surface ice in the area of Chasma Boreale. Hyperboreae Undae, along with Abalos and Siton Undae, contributes sand to mainly medium-density dune fields east of Olympia Undae and extending to the Martian prime meridian,

Image analysis research, using the method of spectral derivatives, has indicated that Hyperboreae Undae, as well as the other dense officially-named northern circumpolar dune fields (Olympia Undae, Abalos Undae, and Siton Undae), show the highest density of gypsum in the area. A geomorphic comparison of Hyperboreae Undae with Rub' al Khali, Earth's largest contiguous dune field, has determined that the morphologies of the two ergs follow similar developmental patterns.

Linear dunes form primarily in bidirectional (bimodal) wind fields. Transverse dunes, also called barchan, form when there is a unidirectional (unimodal) wind regime. A third type of dune, the star dune, is typically formed in multidirectional (multimodal) wind regimes. The presence of each of these dune forms, suggests the wind regime that produced it. Linear and star dunes are rare on Mars. The existence of both linear and barchan dunes in the same location is apparently incompatible, as that would seem to imply the co-existence of unidirectional and bidirectional winds in the same place.

Research has been undertaken to explain the coexistence of linear and barchan dunes in Hyperboreae Undae. One paper explains the change from linear to barchan dunes in adjacent locations, by proposing a wind model that changes from bidirectional to unidirectional due to the influence of local topography; it is proposed that bidirectional winds change to unidirectional due to funneling action introduced by local geomorphology. Although valid for neighbouring dune locations, this theory cannot explain how linear and barchan dunes can coexist in the same location.